Mugrauer, Rück & Michel

M. Mugrauer, Astrophysikalisches Institut und Universitäts-Sternwarte Jena,
Schillergäßchen 2, D-07745 Jena, Germany.

# Gaia Search for stellar Companions of TESS Objects of Interest IV

M. Mugrauer  J. Rück  K.-U. Michel  Astrophysikalisches Institut und
Universitäts-Sternwarte Jena<EMAIL_ADDRESS>
(2023; 2023; 2023)

###### Abstract

We present the latest results of our ongoing multiplicity study of (Community)
TESS Objects of Interest, using astrometric and photometric data from the ESA-
Gaia mission to detect stellar companions of these stars and characterize
their properties.A total of 134 binary, 6 hierarchical triple, and two
quadruple star systems are identified among 1106 targets whose multiplicity is
investigated in the course of our survey, located at distances closer than
about 500 pc around the Sun. The detected companions and targets are at the
same distance and have a common proper motion, as expected for components of
gravitationally bound stellar systems, as demonstrated by their accurate Gaia
DR3 astrometry. The companions have masses from about 0.11 to 2 $M_{\odot}$
and are most abundant in the mass range between 0.2 and 0.5 $M_{\odot}$. The
companions have projected separations from the targets between about 50 and
9700 au. Their frequency is the highest and constant from about 300 up to 750
au, decreasing at larger projected separations. In addition to main sequence
stars, four white dwarf companions are detected in this study, whose true
nature is revealed by their photometric properties.

###### keywords:

binaries: visual, white dwarfs,
stars: individual (TOI 3714 B, TOI 3984 B, TOI 4301 B, CTOI 13073396 B)

††articletype: Article Type

##  1 Introduction

Figure 1: The histograms of the individual properties of the targets in this
study. The histograms of distance ($dist$), total proper motion ($\mu$), and
G-band magnitude are based on the Gaia DR3 data of all 1106 targets. Masses
and effective temperatures ($T_{\rm eff}$) have been taken from the Starhorse
catalog where available, which is the case for 1078 targets.

In 2020 we initiated a new survey at the Astrophysical Institute and
University Observatory Jena with the aim to explore the multiplicity of
(Community) TESS Objects of Interest ((C)TOIs), i.e. stars photometrically
monitored by the Transiting Exoplanet Survey Satellite (TESS, Ricker ., 2015),
which show promising dips in their light curves, possibly caused by exoplanets
orbiting these stars.

In our survey, stellar companions of (C)TOIs are detected and their properties
are determined with astrometry and photometry, originally from the 2nd data
release (Gaia DR2 from hereon, Gaia Collaboration ., 2018) and later from the
early version of the 3rd data release (Gaia EDR3 from hereon, Gaia
Collaboration ., 2021) of the ESA-Gaia mission. The first results of the
survey were presented by Mugrauer Michel (2020), Mugrauer Michel (2021), and
Mugrauer . (2022), who have already examined the multiplicity of more than
4100 (C)TOIs, all of which are listed in the (C)TOI release of the `Exoplanet`
`Follow-up` `Observing` `Program` for TESS (ExoFOP-TESS)111Online available
at:
https://exofop.ipac.caltech.edu/tess/view_toi.php
https://exofop.ipac.caltech.edu/tess/view_ctoi.php. Meanwhile, several of
these (C)TOIs discovered as members of multiple star systems in the course of
our survey have already been confirmed as exoplanet host stars by follow-up
observations, e.g. TOI 179, TOI 277, TOI 954, TOI 1228, TOI 1246, TOI 1410,
TOI 1452, TOI 1516, TOI 1690, TOI 1710, TOI 1749, TOI 1797, TOI 1801, TOI
2152, TOI 2193, and TOI 2459, which are listed in the `Extrasolar Planets
Encyclopaedia` (see Schneider ., 2011, and references therein)222Online
available at: http://exoplanet.eu/.

Thanks to the successful execution of the TESS mission and the photometric
analysis of its data, the number of (C)TOIs, and thus the number of targets
for our survey, is continuously growing. In this paper, we search for
companions of more than thousand (C)TOIs reported by the ExoFOP-TESS, whose
multiplicity has not yet been studied in our survey, using the latest data
release from the ESA-Gaia mission.

In the following section we describe in detail the properties of the selected
targets and the search for companions around these stars. In Section 3 we
present all (C)TOIs with detected companions and characterize the properties
of these stellar systems. Finally, we summarize the current status of our
survey and give an outlook on the project in the last section of this paper.

##  2 Search for stellar companions of (C)TOIs by exploring the Gaia DR3

The companion search presented here uses astrometric and photometric data from
the 3rd data release of the ESA-Gaia mission (Gaia DR3 from hereon, Gaia
Collaboration ., 2022), obtained with the instruments of the ESA-Gaia
satellite during the first 34 months of its mission. This data release
contains astrometric solutions, i.e. position ($\alpha$, $\delta$), parallax
$\pi$, and proper motion ($\mu_{\alpha}\cos(\delta)$, $\mu_{\delta}$) of about
1.5 billion sources down to a limiting magnitude of 21 mag in the G-band,
which means white light observations exploiting the entire spectral
sensitivity range of the used CCD detectors.

Parallaxes are measured with an uncertainty in the range of about 0.02
milliarcsec (mas) for bright ($G<15$ mag, with a lower limit of $G\sim 1.7$
mag) up to 0.5 mas for faint ($G=20$ mag) detected sources. Proper motions are
determined with an accuracy of about 0.02 mas/yr for bright objects,
deteriorating to 0.6 mas/yr for $G=20$ mag. In addition, the G-band magnitude
of all sources is recorded with a photometric uncertainty ranging from about
0.3 millimagnitude (mmag) for the brightest to 6 mmag for faint sources.

In the study presented here, stellar companions of the investigated (C)TOIs
are firstly identified as sources that are at the same distance as the targets
and secondly have a common proper motion with these stars. In order to
unambiguously detect co-moving companions and confirm their equidistance to
the (C)TOIs, we consider in our study only those sources listed in the Gaia
DR3 for which there is a significant measurement of parallax
($\pi/\sigma(\pi)>3$) and proper motion ($\mu/\sigma(\mu)>3$). Sources with a
negative parallax are ignored.

Since our survey was originally based on Gaia DR2 data, with a typical
parallax uncertainty of 0.7 mas for faint sources down to $G=20$ mag, it is
restricted to (C)TOIs within 500 pc of the Sun (i.e. $\pi>2$ mas), to ensure
that $\pi/\sigma(\pi)>3$ also applies to the faintest detectable companions.
This distance constraint is slightly relaxed to $\pi+3\sigma(\pi)>2$ mas, i.e.
the parallax uncertainty of the (C)TOIs is also taken into account. Although
we are now using Gaia DR3 data, which exhibit a smaller parallax uncertainty,
we retain the chosen distance constraint for the survey for continuity.

In this paper, we explore the multiplicity of 1106 targets333The target sample
consists of 747 TOIs and 359 CTOIs, i.e. approximately twice as many TOIs as
CTOIs. The relative frequency of CTOIs among the targets examined here is
about 1.3 times higher than the relative frequency of these objects among the
targets whose multiplicity was previously examined in the course of this
survey. that have not yet been investigated in the course of our survey with
Gaia DR3 data, that meet the distance constraint described above and are
therefore selected as targets for the study presented here. Figure 1
illustrates the properties of the selected targets with histograms. The
distance ($dist$) and total proper motion ($\mu$) of all targets are
determined using their precise Gaia DR3 parallax ($dist[{\rm
pc}]=1000/\pi[{\rm mas}]$) and proper motion in right ascension and
declination. The G-band magnitude of all targets is listed in the Gaia DR3,
while their mass and effective temperature ($T_{\rm eff}$) are taken from the
Starhorse catalog (SHC from here on, Anders ., 2019) where available, which is
the case for 1078 stars, i.e. the vast majority ($\sim 97$ %) of all 1106
targets. The targets have distances from the Sun between about 6 to 840 pc.

The distance distribution of the target sample examined here is rather flat
compared to the distribution of the distance of the targets investigated
earlier in this survey, which shows a peak at about 100 pc. This difference in
distance distribution results from the unequal distance distributions of the
TOIs and CTOIs in the target sample studied here. While the CTOIs have a peak
in their distance distribution at about 100 pc, similar to the targets whose
multiplicity was examined earlier in this survey, the TOIs are located at
greater distances from the Sun and are most frequently found at about 350 pc.
Due to their smaller distance, the CTOIs also appear brighter (by about 1 mag
on median) and have proper motions that are on median about 1.5 times higher
than those of the TOIs.

The targets studied here have proper motions in the range between about 1 and
1660 mas/yr444The median of the proper motion of the targets studied here is
26 mas/yr which is just slightly lower than the median of the proper motion of
the targets studied earlier in this survey ($Mdn(\mu)=32$ mas/yr)., G-band
magnitudes from 3.4 to 17 mag555The targets whose multiplicity is investigated
here have a G-band magnitude of 12 mag on median which is one magnitude
fainter than the median magnitude of the targets studied before in the course
of this survey. masses between about 0.14 and 3.8 $M_{\odot}$, and effective
temperatures ranging from about 2700 up to 10100 K. Based on the cumulative
distribution functions of the individual properties, the targets are most
commonly located at distances between about 50 and 500 pc have typical proper
motions from about 5 to 30 mas/yr, and G-band magnitudes from about $G=11$ to
14 mag. The targets are mainly solar-like stars with masses in the range
between about 0.7 and 1.3 $M_{\odot}$. This population is also evident in the
$T_{\rm eff}$-distribution of the targets at intermediate temperatures around
4500 to 6500 K. An additional but weaker clustering of targets is found in
this distribution at lower effective temperatures between about 3400 and 4400
K, namely the early M to mid K dwarf population.

As defined and described in Mugrauer Michel (2020), our survey is restricted
to companions with projected separations up to 10000 au, which on the one hand
guarantees an effective companion search, but on the other hand also detects
the vast majority of all wide companions of the selected targets. This results
in an angular search radius for companions around the targets of $r[{\rm
arcsec}]=10\pi[{\rm mas}]$, with $\pi$ the Gaia DR3 parallax of the (C)TOIs.

All sources listed in Gaia DR3 that are located within the search radius used
around the targets and have a significant parallax and proper motion are
considered companion-candidates. A total of about 33000 such objects are
detected around 891 targets, whose multiplicity is investigated in this study.
The companionship of all these candidates is tested using their precise Gaia
DR3 astrometry and that of the associated (C)TOIs, following exactly the
procedure described in Mugrauer Michel (2020). The vast majority of these
sources can be excluded as companions because they do not have have a common
proper motion with the (C)TOIs and/or are not at the same distance as these
stars. In contrast, 149 candidates can be unambiguously confirmed as
companions of the (C)TOIs with their accurate Gaia DR3 astrometry. The
properties of these companions and the associated (C)TOIs are described in
detail in the next section of this paper.

Figure 2: The $T_{\rm eff}$-$M_{\rm G}$-diagram of (C)TOIs with detected
companions presented here. (C)TOIs listed in the SHC with surface gravities
$\log(g[\rm{cm/s^{-2}}])<3.8$ are shown as red circles, those with larger
surface gravities with black circles, respectively. The main sequence is
plotted as a grey dashed line.

##  3 (C)TOIs and their detected stellar companions

The mass, effective temperature and absolute G-band magnitude of most of the
(C)TOIs with detected companions presented here are listed in the SHC, and we
show these stars in a $T_{\rm eff}$-$M_{\rm G}$-diagram in Figure 2. In this
diagram we plot the main sequence of Pecaut Mamajek (2013)666Online available
at: http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt.
Version 2022.04.16 is used here. for comparison.

Most targets with detected companions are main sequence stars. Only a few
(C)TOIs are (significantly) located above the main sequence, and these stars
also have surface gravities of $\log(g[\rm{cm/s^{-2}}])<3.8$, as listed in the
SHC, and are therefore classified as (sub)giants.

The parallax, proper motion, apparent G-band magnitude, and extinction
estimate of the (C)TOIs and their companions detected in this study are
summarized in Table 3,which lists a total of 134 binary, 6 hierarchical
triple, and two quadruple star systems.

We determine the angular separation ($\rho$) and the position angle ($PA$) of
all detected companions to the associated (C)TOIs, using the precise Gaia DR3
astrometry of each object. The derived relative astrometry of the companions
is listed in Table 4, together with its uncertainty, which remains below about
1.3 mas in angular separation or 0.08 ∘ in position angle.

Table 4 also summarizes the parallax difference $\Delta\pi$ between the
(C)TOIs and their companions, together with its significance
$sig\text{-}\Delta\pi$, which is also calculated taking into account the
astrometric excess noise of each object. The same table lists for each
companion its differential proper motion $\mu_{\rm rel}$ relative to the
associated (C)TOI with its significance, and its $cpm$-$index$777The common
proper motion ($cpm$) index, as defined in Mugrauer Michel (2020),
characterizes the degree of common proper motion of a detected companion with
the associated (C)TOI..

The parallaxes of the individual components of the stellar systems presented
here are not significantly different from each other
($sig\text{-}\Delta\pi<3$) when the astrometric excess noise is taken into
account. This clearly proves the equidistance of the detected companions with
the (C)TOIs, as expected for components of physically associated stellar
systems. All but one of the detected companions have a $cpm\text{-}index\geq
5$ and more than 95 % of them even have a $cpm\text{-}index\geq 10$, i.e. the
detected companions and the associated (C)TOIs clearly form common proper
motion pairs, as expected for gravitationally bound stellar systems. Note that
for systems with small $cpm$-$index$ and parallax, the possibility of random
pairing is increased.

Table 1: Photometry of three white dwarf companions detected in this study. For each companion we list the color difference $\Delta(B_{\rm P}-R_{\rm P})$ and the G-band magnitude difference $\Delta G$ to the associated (C)TOI, its apparent $(B_{\rm P}-R_{\rm P})$ color, as well as its derived intrinsic color $(B_{\rm P}-R_{\rm P})_{0}$ and effective temperature $T_{\rm eff}$. Companion | $\Delta G$ | $\Delta(B_{\rm P}-R_{\rm P})$ | $(B_{\rm P}-R_{\rm P})$ | $(B_{\rm P}-R_{\rm P})_{0}$ | $T_{\rm eff}$
---|---|---|---|---|---
| [mag] | [mag] | [mag] | [mag] | [K]
TOI 3714 B | $4.557\pm 0.004$ | $-1.217\pm 0.078$ | $1.100\pm 0.078$ | $0.859_{-0.243}^{+0.110}$ | $5632^{+809}_{-316}$
TOI 3984 B | $4.433\pm 0.005$ | $-1.957\pm 0.099$ | $0.557\pm 0.099$ | $0.440_{-0.128}^{+0.128}$ | $6999^{+615}_{-393}$
CTOI 13073396 B | $2.651\pm 0.004$ | $-2.356\pm 0.011$ | $0.138\pm 0.009$ | $-0.060_{-0.035}^{+0.043}$ | $10015^{+450}_{-512}$

As we use astrometric data from the latest Gaia data release in this study, it
is worth noting that the equidistance and common proper motion of all but two
of the companions previously detected in this survey using Gaia DR2 astrometry
(see Mugrauer Michel, 2020), are confirmed by Gaia DR3 astrometry. While the
$cpm$-$index$ of almost all companions remains constant, the parallax
difference between the detected companions and the (C)TOIs is reduced to about
half with the more accurate Gaia DR3 astrometry, reinforcing the conclusion
that these co-moving companions and the (C)TOIs are components of physically
associated stellar systems. For TOI 737 B and TOI 851 B, their companionship
could not be tested with Gaia DR3 astrometry because only their equatorial
coordinates, but not their proper motion or parallax, are listed in the latest
Gaia data release. However, according to their Gaia DR2 astrometry, both
companions have a high degree of common proper motion ($cpm$-$index$ of 29 and
57, respectively), and their differential proper motion does not significantly
exceed the expected escape velocity. We therefore conclude that also these two
stars are gravitationally bound companions of the associated TOIs.

Figure 3: This $T_{\rm eff}$-$M_{\rm G}$-diagram shows all detected companions
whose effective temperatures are listed in either the SHC or SHC2, or for
which Apsis-Priam temperature estimates are available. Companions, which are
the primary components of their stellar systems, are shown as green star
symbols. The main sequence is plotted as a dashed grey line for comparison.
Figure 4: (RGB)-color-composite images of TOI 3714, TOI 3984 and CTOI 13073396
with their white dwarf companions from y-, i- and g-band Pan-STARRS images.

The absolute G-band magnitudes of all detected companions are from the SHC or,
if not available, from the SHC2 (Anders ., 2022), indicated with the SHC2 flag
in Table 5.

The SHC is based on several photometric catalogues as well as on Gaia DR2
astrometry and photometry, the SHC2 on the corresponding data of the Gaia
EDR3. Where possible, we use the data from the SHC instead of the SHC2, since
the properties of a larger number of detected companions but also (C)TOIs are
listed in this catalogue than in the SHC2.

If the absolute magnitude of the companions is not listed in these catalogs,
it is derived using the apparent G-band photometry of the companions as well
as the parallax of the (C)TOIs, and the Apsis-Priam G-band extinction estimate
listed in the Gaia DR2 if available, otherwise the G-band extinction from the
SHC. The companion extinction estimate is used if available, otherwise that of
the (C)TOIs.

The projected separation of all companions is determined from their angular
separation from the associated (C)TOIs and the parallax of these stars.

The mass and effective temperature of the companions presented here, including
their uncertainties, are from the SHC or the SHC2 (indicated by the SHC2 flag
in Table 5) where available, which is the case for about 73 % of all
companions. We plot these companions in Figure 3 in a $T_{\rm eff}$-$M_{\rm
G}$-diagram, along with the companions for which an Apsis-Priam estimate of
their effective temperature is available888As recommended by Andrae . (2018),
we only use Apsis-Priam temperature estimates in this survey if their flags
are equal to 1A000E where A and E can have any value., as indicated by the PRI
flag in Table 5. The photometry of all these companions is in good agreement
with that expected for main sequence stars.

For the remaining 40 companions their mass and effective temperature are
derived from their absolute G-band magnitude by interpolation (inter flag in
Table 5) using the $M_{\rm G}$-mass\- and $M_{\rm G}$-$T_{\rm eff}$-relation
from Pecaut Mamajek (2013), assuming that these companions are main sequence
stars. To test this hypothesis, we compare the obtained effective temperature
of the companions either with their Apsis-Priam temperature estimate, if
available, or with the effective temperature of the companions inferred from
their $(B_{\rm P}-R_{\rm P})$ color and reddening estimate $E(B_{\rm P}-R_{\rm
P})$999The reddening of an object is estimated from its extinction $A_{\rm G}$
using the relation $A_{\rm G}/E(B_{\rm P}-R_{\rm P})=1.89$ from Wang Chen
(2019)., using the $(B_{\rm P}-R_{\rm P})_{0}$-$T_{\rm eff}$-relation from
Pecaut Mamajek (2013).

For all but three of these companions their effective temperature, determined
from their absolute magnitude under the assumption that they are main sequence
stars, agrees well with their Apsis-Priam temperature estimate or with the
temperature derived from their color. The typical deviation of the different
temperature estimates is about 430 K, which is in good agreement with the
precision of the derived effective temperatures. We therefore conclude that
these companions are all main sequence stars.

In addition, we also compare the Gaia DR3 $(B_{\rm P}-R_{\rm P})$ color of the
(C)TOIs and their companions (if any), indicated by the BPRP flag in Table 5.
For main sequence stars companions, fainter/brighter than the (C)TOIs, are
expected to appear redder/bluer than the stars, and this is true for most of
the detected companions, except for TOI 3714 B, TOI 3984 B, and CTOI 13073396
B. These three companions are also observed with the Panoramic Survey
Telescope and Rapid Response System (Pan-STARRS) and their y-, i-,g-band
color-composite images are shown in Figure 4. In these images the faint
companions are clearly visible as bluish sources next to the associated much
brighter (C)TOIs.

The photometric properties of these companions are summarized in Table 1. The
companions are several magnitudes fainter than the (C)TOIs but appear bluer
than these stars. The temperatures of the companions inferred from their
colors are significantly higher (by about 2700 to 6900 K) than the
temperatures, derived from their absolute G-band magnitudes, assuming that
they are main sequence stars.

Figure 5: $T_{\rm eff}$-$M_{\rm G}$-diagram of the stellar systems with white
dwarf components detected in this study. The main sequence is shown as a grey
dashed line and the evolutionary mass tracks of DA white dwarfs with masses of
0.5 and 0.6 $M_{\odot}$ as black dotted lines. The primaries of the systems
are plotted as white circles, the white dwarf secondaries as black circles,
respectively. Figure 6: TOI 4301 A (center of all images) and its co-moving
white dwarf companion TOI 4301 B imaged with the UK Schmidt Telescope (UKST)
in the filters GG 395 (Blue) and RG 610 (Red), respectively. The companion is
well detected in the blue spectral range, but becomes fainter towards longer
wavelengths and is not visible in the 2MASS Ks-band image. The expected
position of TOI 4301 B in this image is marked with a black circle. Next to
this position is the star 2MASS 11050267-4602149, which is indicated with a
black arrow in all images.

Figure 5 shows these companions together with the other components of their
stellar systems in a $T_{\rm eff}$-$M_{\rm G}$-diagram. For comparison, we
plot the main sequence from Pecaut Mamajek (2013) in this diagram, and the
mass tracks for DA white dwarfs from the Bergeron et al. evolutionary models
of white dwarfs (for further details see Bédard ., 2020; Bergeron ., 2011;
Blouin ., 2018; Holberg Bergeron, 2006; Kowalski Saumon, 2006 and Tremblay .,
2011)101010Online available at:
https://www.astro.umontreal.ca/~bergeron/CoolingModels/. Version 2021.01.13 is
used here.. While the brighter primary components of these systems are all
main sequence stars, the faint secondaries are well below the main sequence,
and their Gaia photometry best matches that expected for white dwarfs. We
therefore conclude that these companions are white dwarfs, as indicated by the
WD flag in Table 5.

Figure 7: The histograms of the properties of the companions detected in this
study.

Another white dwarf companion is revealed in this project due to its intrinsic
faintness. TOI 4301 B has an absolute G-band magnitude of $M_{\rm
G}=13.21^{+0.08}_{-0.1}$ mag and a magnitude difference of $\Delta G=8.458\pm
0.005$ mag to the associated potential exoplanet host star TOI 4301 A.
Although there is no color information for TOI 4301 B in the Gaia DR3, the
white dwarf nature of this companion can be deduced from its photometric
properties. While TOI 4301 B is visible in the optical spectral range and is
listed in the Gaia DR3, it is not detected in the 2MASS Ks-band image which is
shown in Figure 6. In this figure, the expected position of the companion at
the 2MASS observing epoch (February 2000) is indicated by a black circle,
calculated using the Gaia DR3 astrometry of the companion and the epoch
difference between the 2MASS observation and the Gaia DR3 reference epoch
(2016.0). The 2MASS image has a $S/N=10$ detection limit of about 14.9 mag.
Near the position of the companion, the star 2MASS 11050267-4602149
($Ks=14.6\pm 0.1$ mag, Skrutskie ., 2006) is well detected in the 2MASS image,
consistent with the given detection limit. If TOI 4301 B were a main sequence
star, we would expect its apparent Ks-band magnitude to be $Ks=14.5\pm 0.1$
mag, derived from the photometric data of main sequence stars from Pecaut
Mamajek (2013), using the G-band photometry of the companion, the extinction
in this band, the given extinction relations $A_{\rm G}/A_{\rm V}=0.789$ and
$A_{\rm Ks}/A_{\rm V}=0.078$ from Wang Chen (2019), and the parallax of TOI
4301. Therefore, if the companion were a main sequence star, it should be
clearly visible in the 2MASS image, similar like 2MASS 11050267-4602149. In
contrast, if the companion were a white dwarf, we could infer its expected Ks-
band photometry as above, but using the evolutionary DA white dwarf models of
Bergeron et al. instead. For an assumed companion mass of 0.6 $M_{\odot}$ we
obtain $Ks\sim 18.3$ mag, which is clearly below the 2MASS detection limit. We
therefore conclude that TOI 4301 B is a white dwarf, due to its intrinsic
faintness in the optical and near-infrared spectral range. With the assumed
mass of this degenerated companion and the white dwarf evolutionary models
mentioned above, the absolute G-band photometry of the companion yields its
effective temperature, which is $T_{\rm eff}=7447^{+211}_{-158}$ K.

Figure 7 shows the histograms of the properties of all companions detected in
this project. The companions have angular separations to the (C)TOIs, ranging
from about 0.4 to 167 arcsec, corresponding to projected separations from 51
up to 9736 au. According to the underlying cumulative distribution function,
the frequency of the companions is highest and constant between about 300 and
750 au, decreasing for larger projected separations. Half of all companions
have projected separations of less than 1500 au. In total, 5 stellar systems
(four binaries, and one hierarchical triples) with projected separations below
200 au are detected, namely: TOI 3073 AB, TOI 3634 AB, TOI 4175 AB+C, TOI 4349
AB, and CTOI 248960573 AB, i.e. the most challenging environments for planet
formation identified in this study.

The companion masses range from about 0.11 to 2 $M_{\odot}$ (the mean mass is
$\sim 0.6\,M_{\odot}$). The highest companion frequency in the cumulative
distribution function is found in the mass range between 0.2 and 0.5
$M_{\odot}$, corresponding to mid to early M dwarfs, according to the relation
between mass and spectral type (SpT) from Pecaut Mamajek (2013). For higher
masses, the companion frequency is lower but constant between about 0.7 and
1.1 $M_{\odot}$, from where it decreases continuously towards higher masses.
This peak in the companion population is also seen in the distribution of
their effective temperature, where the companion frequency is highest at
temperatures between about 3200 and 3700 K. There is also a second but weaker
clustering of companions between about 4600 and 6100 K, corresponding to mid K
to late F-type stars, according to the $T_{\rm eff}$-SpT-relation from Pecaut
Mamajek (2013).

As can be seen from the separation-mass-diagram in Figure 8, of the 149
companions presented here, 18 are the primary, 124 are the secondary, 5 the
tertiary, and 2 the quaternary component of their stellar systems.

Figure 8: The separation-mass-diagram of the companions detected in this
study. Companions that are the primary components of their stellar systems are
shown as star symbols, secondaries as grey circles, tertiary components as
black triangles, and quaternary components as black squares, respectively.
Detected white dwarf companions, assumed to have a mass of 0.6 $M_{\odot}$,
are plotted as white crossed circles (note that the symbols of the white dwarf
companions TOI 4301 B, and CTOI 13073396 B overlap at a separation of about
5000 au). Figure 9: The magnitude difference of all detected companions
plotted against their angular separation from the associated (C)TOI. The Gaia
detection limit, found by Mugrauer . (2022), is shown as a dotted line for
comparison. The expected average magnitude differences for companions with 0.1
or 0.6 $M_{\odot}$ are shown as grey dashed horizontal lines. Figure 10:
(RGB)-color-composite images of the hierarchical quadruple system TOI 3106
AC+BD, and of the triple system TOI 3584 AB+C from z- (or y-), i-, and g-band
Pan-STARRS images. A detailed y-band Pan-STARRS image is shown for TOI 3548
AB+C, in which the primary and secondary component of this triple star system
are well resolved. The (RGB)-color-composite images of the binary systems TOI
4001 AB, and TOI 4079 BA, are composed of R-, V-, and B-band images taken with
the CTK-II at the University Observatory Jena.

To characterize the detection limit reached in this project, we plot the
magnitude difference of all detected companions over their angular separation
to the associated (C)TOIs, as shown in Figure 9. For comparison, we plot the
Gaia detection limit determined by Mugrauer . (2022), which agrees well with
the detection limit presented here. Only at small angular separations below
about 0.4 arcsec does it seem to be too conservative. In this angular
separation range one companion is detected that is about 0.4 mag fainter than
the associated TOI.

The expected brightness difference between the targets of this study and low-
mass main sequence companions (shown as grey dashed lines in Figure 9) is
estimated using the expected absolute G-band magnitude of these stars, as
listed in Pecaut Mamajek (2013), and the average absolute G-band magnitude of
our targets ($M_{\rm G}\sim 4.2$ mag). As shown in Figure 9, a magnitude
difference of about 3.7 mag is reached at an angular separation of about 0.9
arcsec around the targets of this project. This allows the detection of
companions with masses down to about 0.6 $M_{\odot}$ (mean mass of all
detected companions) that are separated from the (C)TOIs by more than 250 au.
In addition, companions with masses down to about 0.1 $M_{\odot}$ are
detectable beyond 4 arcsec, corresponding to a projected separation of 1100 au
at the average target distance of 280 pc.

##  4 Summary and Outlook

In recent years, several surveys have been carried out using ground-based
observations to explore the multiplicity of exoplanet host stars (see e.g.
Mugrauer Ginski, 2015; Ginski ., 2021). Here we present the latest results of
our survey based on data of the ESA-Gaia mission, which was initiated at the
University Observatory Jena in early 2020 with the aim of detecting and
characterizing stellar companions of (C)TOIs, i.e. potential exoplanet host
stars. In the study presented in this paper we search for companions of 1106
(C)TOIs announced in the (C)TOI release of the ExoFOP-TESS, whose multiplicity
has not yet been investigated in the course of our survey, using Gaia DR3
data.

In total, about 33000 sources with accurate astrometric solutions are detected
in the Gaia DR3 around 891 targets, while around the remaining 215 targets of
this survey no companion-candidates are identified within the applied search
radius. In total, new co-moving companions are detected around 142 of all
targets whose multiplicity is studied here. In addition, companions around a
further 23 (C)TOIs are found in the Gaia DR3, but these had already been
detected in the Gaia DR2 by Mugrauer (2019), Mugrauer Michel (2020), and
Michel Mugrauer (2021). Thus, the multiplicity rate of the investigated
(C)TOIs is at least $14.9\pm 1.1$ %, which is lower than the rate found in our
survey so far (e.g. $20.1\pm 0.9$ %, Mugrauer ., 2022). The reason for this
difference is the low multiplicity rate of the CTOIs examined in this study,
which is only about 5 %. In contrast, the multiplicity rate of the TOIs is
$19.9\pm 1.5$ %, which is well in line with the multiplicity rates found
earlier in our survey. As described above, the CTOIs whose multiplicity is
studied here are closer to the Sun than the TOIs. A smaller distance usually
leads to higher proper motion, brightness and angular separation of potential
companions, which should facilitate their detection. Therefore, the
surprisingly low multiplicity rate of the CTOIs found in this study must be an
effect of the target selection by the ExoFOP-TESS.

Color-composite images of some of the detected stellar systems are shown in
Figure 10, taken with Pan-STARRS or with the Cassegrain-Teleskop-Kamera (CTK-
II, Mugrauer, 2016) at the University Observatory Jena. In addition to 134
binaries, two quadruple star systems are revealed in which the (C)TOIs have
both a close companion and a distant binary companion. Furthermore, three
hierarchical triple star systems are detected, whose individual components are
listed in the Gaia DR3. Moreover, significant ($Mdn(sig)=20$) astrometric non-
single-star solutions are listed in the Gaia DR3 for the co-moving companions
of TOI 3875, TOI 4128, and TOI 4420 (indicated with the NSS flag in Table 5).
For the companions of TOI 3875 and TOI 4128, a Keplerian orbital motion of
their photocenter is detected in the Gaia astrometry ($P=502.5\pm 5.0$ days,
$a=0.99\pm 0.05$ mas, $e=0.36\pm 0.10$, $i=86.9\pm 2.5$ ∘ for TOI 3875 B, and
$P=802.7\pm 11.2$ days, $a=1.86\pm 0.03$ mas, $e=0.61\pm 0.02$, $i=129.1\pm
1.2$ ∘ for TOI 4128 B, respectively). So these companions are themselves close
binary systems. With the masses of TOI 3875 B and TOI 4128 B, and their Gaia
DR3 parallaxes redetermined in the non-single star solutions ($\pi=2.482\pm
0.026$ mas for TOI 3875 B, and $\pi=3.210\pm 0.017$ mas for TOI 4128 B,
respectively), the masses of the unseen tertiary components and the semi-major
axis of these close binary systems can be determined. We obtain $0.37\pm
0.03\,M_{\odot}$ for the mass of TOI 3875 C, and $0.38\pm 0.02\,M_{\odot}$ for
TOI 4128 C, respectively. The semi-major axis of the TOI 3875 BC system is
$a=1.33\pm 0.03$ au, which corresponds to about 3 mas at the distance of the
system, and $a=1.78\pm 0.05$ au ($\sim 6$ mas) for TOI 4128 BC, respectively.
The companion of TOI 4420 is identified as a single-lined spectroscopic binary
in the Gaia DR3. According to its significant ($sig=12$) orbital solution, the
companion has a radial velocity (RV) semi-amplitude of $K=20.9\pm 1.8$ km/s, a
period of $P=4.7257\pm 0.0009$ days, and an eccentricity of $e=0.24\pm 0.09$.
Together with the mass of TOI 4420 B this gives the minimum-mass of the
unresolved companion TOI 4420 C ($\sim 0.16\,M_{\odot}$), and the minimum of
the semi-major axis of this close binary system ($\sim 0.05$ au). Thus, TOI
3875, TOI 4128, and TOI 4420 are three more hierarchical triples composed of
the TOIs and their distant binary companions. Hence, a total of 6 hierarchical
triple star systems are detected in the multiplicity study presented here.

Furthermore, the companion TOI 3956 A, is listed in the Gaia DR3 as having a
significant acceleration of its proper motion ($\dot{\mu}=1.22\pm 0.04$
mas/yr2), i.e. this star probably has an additional close stellar companion
with an orbital period longer than the 34-months period on which the Gaia DR3
is based on. We therefore classify TOI 3956 as a potential hierarchical triple
star system, whose triple nature will have to be confirmed by follow-up
observations.

As expected for components of stellar systems the (C)TOIs and the detected
companions are equidistant and share a common proper motion, as verified by
their accurate Gaia DR3 parallax and proper motion. In particular, the direct
proof of the equidistance of the individual components of the stellar systems,
as done in this study by comparing their parallax, was not possible in
previous multiplicity surveys prior to the release of the precise Gaia data,
because in particular for most of the faint companions their parallax could
not be measured by the ESA-Hipparcos mission (Perryman ., 1997).

However, 23 companions identified in this project are already listed in the
WDS, either as co-moving companions or as companion-candidates of the (C)TOIs,
requiring confirmation of their companionship, which is finally provided by
this study. Although the WDS is currently the most complete catalog of
multiple star systems available, containing relative astrometric measurements
of multiple star systems over a period of more than 300 years, 126 (i.e. about
84 % of all) companions not listed in the WDS are detected in this project and
are marked with the $\bigstar$ flag in Table 4. This demonstrates the great
potential of the ESA-Gaia mission for the study of stellar multiplicity,
especially for the detection of wide companions, as shown by the derived
detection limit of this study in Figure 9. On average, all stellar companions
with masses down to about 0.1 $M_{\odot}$ are detectable around the targets in
this study beyond about 4 arcsec (or 1100 au of projected separation), and
more than half of all detected companions have such separations. Overall,
companions with projected separations between about 50 and 9700 au are
detected, and the frequency of companions is constant and highest for
separations between about 300 and 750 au, while it decreases significantly for
larger projected separations. The companions found in this project have masses
ranging from about 0.11 to 2 $M_{\odot}$ and are most abundant in the mass
range between 0.2 and 0.5 $M_{\odot}$. In addition to main sequence stars,
four white dwarfs are identified as co-moving companions of the (C)TOIs, whose
true nature is revealed based on their photometric properties.

A significant ($sig\text{-}\mu_{\rm rel}\geq 3$) differential proper motion
$\mu_{\rm rel}$ relative to the associated (C)TOIs is detected for 122 (i.e.
about 80 % of all) companions presented here. We derive the escape velocity
$\mu_{\rm esc}$ of all these companions using the approximation described in
Mugrauer (2019). The differential proper motion of most of these companions is
consistent with orbital motion. In contrast, the differential proper motion of
19 companions significantly exceeds the expected escape velocity. Since these
companions all have a high degree of common proper motion
($cpm\text{-}index\geq 10$), this may indicates a higher degree of
multiplicity as described in Mugrauer (2019). In fact, five of the companions
are members of already confirmed hierarchical triple or quadruple star
systems. For the companion TOI 3956 A, a significant acceleration of its
proper motion is listed in the Gaia DR3, indicating that this star is itself a
close binary, i.e. TOI 3956 is a potential hierarchical triple star system.
Follow-up (high contrast imaging) observations are needed to further
investigate the multiple status of all these particular systems and their
companions, which are summarized in Table 2.

Table 2: List of all detected companions (sorted by their identifier) whose differential proper motion $\mu_{\rm rel}$ relative to the (C)TOIs significantly exceeds the expected escape velocity $\mu_{\rm esc}$. Companions already known to be members of hierarchical triple or quadruple star systems are labelled with $\bigstar\bigstar\bigstar$ or $\bigstar\bigstar\bigstar\bigstar$, those in potential triple star systems with $(\bigstar\bigstar\bigstar)$, respectively. Companion | $\mu_{\rm rel}$ | $\mu_{\rm esc}$ |
---|---|---|---
| [mas/yr] | [mas/yr] |
TOI 2690 D | $2.41\pm 0.06$ | $0.66\pm 0.04$ | $\bigstar\bigstar\bigstar\bigstar$
TOI 2774 B | $1.07\pm 0.10$ | $0.34\pm 0.01$ |
TOI 2816 A | $0.49\pm 0.02$ | $0.36\pm 0.02$ |
TOI 3039 B | $3.72\pm 0.35$ | $0.23\pm 0.01$ |
TOI 3106 B | $7.69\pm 0.17$ | $0.48\pm 0.01$ | $\bigstar\bigstar\bigstar\bigstar$
TOI 3106 D | $7.91\pm 0.36$ | $0.41\pm 0.01$ | $\bigstar\bigstar\bigstar\bigstar$
TOI 3314 B | $1.08\pm 0.11$ | $0.55\pm 0.05$ |
TOI 3353 B | $2.67\pm 0.04$ | $1.42\pm 0.05$ |
TOI 3560 B | $1.28\pm 0.14$ | $0.40\pm 0.02$ |
TOI 3628 C | $2.09\pm 0.33$ | $0.39\pm 0.02$ | $\bigstar\bigstar\bigstar$
TOI 3682 B | $5.32\pm 0.05$ | $0.32\pm 0.02$ |
TOI 3781 B | $1.33\pm 0.04$ | $0.67\pm 0.01$ |
TOI 3829 B | $3.00\pm 0.11$ | $1.25\pm 0.05$ |
TOI 3889 B | $1.92\pm 0.03$ | $1.36\pm 0.03$ |
TOI 3956 A | $1.18\pm 0.03$ | $0.67\pm 0.02$ |  $(\bigstar\bigstar\bigstar$)
TOI 4021 B | $1.00\pm 0.02$ | $0.35\pm 0.01$ |
TOI 4175 C | $4.50\pm 0.05$ | $2.49\pm 0.09$ | $\bigstar\bigstar\bigstar$
TOI 4179 A | $6.14\pm 0.25$ | $1.92\pm 0.10$ |
TOI 4370 B | $1.08\pm 0.09$ | $0.65\pm 0.03$ |

In addition to astrometry, also RV data can be used to check the companionship
of the components of stellar systems. For common proper motion pairs, we do
not expect significant differences between the RVs of their components, since
their orbital motion (especially for wide ones) around their barycenter is
typically much smaller than the systematic velocity. For 59 companions
detected in this study (i.e. less than 40 % of all) a comparison between their
RV and that of the associated (C)TOI is possible in the Gaia DR3. As expected,
the RVs of most of these companions and the (C)TOIs do not significantly
deviate from each other. Only four companions have significant RV deviations,
namely: TOI 3956 A ($8.35\pm 2.70$ km/s), TOI 4175 B ($1.98\pm 0.60$ km/s),
TOI 4179 A ($2.34\pm 0.36$ km/s), and TOI 4420 B ($14.99\pm 4.01$ km/s). This
may indicate the presence of additional close stellar companions in these
systems that induce faster orbital motions. This is particulary the case for
companions, belonging to stellar systems whose components have a high degree
of common proper motion, as is the case for the four companions mentioned
above ($cpm\text{-}index\geq 16$). The companions TOI 3956 A, and TOI 4420 B
both have non-single star solutions in the Gaia DR3, so are themselves close
binary systems. TOI 4175 B is a member of a hierarchical triple star system
whose components are resolved by Gaia, and TOI 4179 A is a member of a
potential triple star system according to its Gaia DR3 astrometry.

As demonstrated with the target sample studied here, even in the latest data
release of the ESA-Gaia mission, RVs are available for only a minority of the
detected companions. For this reason, we do not use RV data for companionship
verification in this survey so far, but will include it as soon as it is
available for most of the detected companions, which is expected for the
upcoming Gaia data releases.

The survey, whose latest results are presented here, is an ongoing project
whose target list is continually growing as a result of the ongoing analysis
of photometric data collected by the TESS mission. The multiplicity of all
these newly detected (C)TOIs will be explored in the course of this survey,
and the detected companions and their determined properties will be reported
regularly in this journal and also published online in the `VizieR` database
(Ochsenbein ., 2000)111111Online available at:
https://vizier.u-strasbg.fr/viz-bin/VizieR, and on the website of this
survey121212Online available at: https://www.astro.uni-
jena.de/Users/markus/Multiplicity_of_(C)TOIs.html. The results of this survey,
combined with those of high-contrast imaging observations of the (C)TOIs,
which can detect close companions with projected separations down to only a
few au, will complete our knowledge of the multiplicity of all these potential
exoplanet host stars.

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## Acknowledgments

We used data from:

(1) 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). The DPAC is funded by
national institutions, in particular those participating in the Gaia
Multilateral Agreement.

(2) the `Exoplanet Follow-up Observing Program` website, operated by the
California Institute of Technology, on behalf of the National Aeronautics and
Space Administration under the Exoplanet Exploration Program.

(3) the `Simbad` and `VizieR` databases operated at the CDS in Strasbourg,
France.

(4) the `Extrasolar Planets Encyclopaedia`.

(5) the Pan-STARRS1 surveys, made possible by contributions from the Institute
for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the
Max-Planck Society and its participating institutes, the Max Planck Institute
for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial
Physics, Garching, The Johns Hopkins University, Durham University, the
University of Edinburgh, the Queen’s University Belfast, the Harvard-
Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global
Telescope Network Incorporated, the National Central University of Taiwan, the
Space Telescope Science Institute, and the National Aeronautics and Space
Administration under Grant No. NNX08AR22G issued through the Planetary Science
Division of the NASA Science Mission Directorate, the National Science
Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand
University (ELTE), and the Los Alamos National Laboratory. The Pan-STARRS1
Surveys are archived at the Space Telescope Science Institute (STScI) and are
available through MAST, the Mikulski Archive for Space Telescopes. Additional
support for the Pan-STARRS1 public science archive is provided by the Gordon
and Betty Moore Foundation.

(6) the Second Palomar Observatory Sky Survey (POSS-II), made by the
California Institute of Technology with funds from the National Science
Foundation, the National Geographic Society, the Sloan Foundation, the Samuel
Oschin Foundation, and the Eastman Kodak Corporation. The UK Schmidt Telescope
was operated by the Royal Observatory Edinburgh, with funding from the UK
Science and Engineering Research Council (later the UK Particle Physics and
Astronomy Research Council), until 1988 June, and thereafter by the Anglo-
Australian Observatory. The blue plates of the southern Sky Atlas and its
Equatorial Extension (together known as the SERC-J), as well as the Equatorial
Red (ER), and the Second Epoch [red] Survey (SES) were all taken with the UK
Schmidt. Supplemental funding for sky-survey work at the ST ScI is provided by
the European Southern Observatory. The Digitized Sky Surveys were produced at
the Space Telescope Science Institute under U.S. Government grant NAG W-2166.
The images of these surveys are based on photographic data obtained using the
Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The
plates were processed into the present compressed digital form with the
permission of these institutions.

(7) the Two Micron All Sky Survey, a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation.

(8) the University Observatory Jena, which is operated by the Astrophysical
Institute of the Friedrich-Schiller-University.

Table 3: This table summarizes for all (C)TOIs (listed first) and their
detected co-moving companions their Gaia DR3 parallax $\pi$, proper motion
$\mu$ in right ascension and declination, astrometric excess noise $epsi$,
G-band magnitude, as well as the used Apsis-Priam G-Band extinction estimate
$A_{\rm G}$ or if not available the G-Band extinction, listed in the SHC.

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
2689 A | $3.1299\pm 0.0125$ |  $5.403\pm 0.013$ | $-27.899\pm 0.014$ | 0.000 | $13.2169\pm 0.0028$ |  |
2689 B | $3.1764\pm 0.0394$ |  $5.407\pm 0.041$ | $-28.029\pm 0.043$ | 0.000 | $16.1522\pm 0.0028$ | $0.8067^{+0.3850}_{-0.2357}$ |
2690 B | $4.5220\pm 0.0200$ | $10.420\pm 0.024$ | $-8.449\pm 0.020$ | 0.126 | $11.6878\pm 0.0028$ | $0.0190^{+0.2290}_{-0.0110}$ |
2690 A | $4.5704\pm 0.0175$ | $10.378\pm 0.019$ | $-8.891\pm 0.017$ | 0.098 | $10.0158\pm 0.0028$ | $0.7493^{+0.2668}_{-0.2786}$ |
2690 C | $4.6961\pm 0.0299$ | $11.071\pm 0.032$ | $-7.888\pm 0.032$ | 0.185 | $12.4131\pm 0.0035$ |  |
2690 D | $4.4724\pm 0.0487$ | $12.827\pm 0.050$ | $-8.404\pm 0.047$ | 0.353 | $13.5936\pm 0.0029$ |  |
2713 A | $4.0423\pm 0.0125$ | $-15.172\pm 0.011$ | $-14.971\pm 0.011$ | 0.000 | $13.0583\pm 0.0028$ | $0.1872^{+0.0938}_{-0.1692}$ |
2713 B | $4.0369\pm 0.0489$ | $-15.679\pm 0.044$ | $-15.446\pm 0.044$ | 0.000 | $16.3996\pm 0.0030$ |  |
2774 A | $1.9516\pm 0.0692$ | $-7.016\pm 0.057$ | $-2.619\pm 0.050$ | 0.585 | $13.2880\pm 0.0029$ |  |
2774 B | $1.9328\pm 0.0957$ | $-8.056\pm 0.081$ | $-2.374\pm 0.070$ | 0.753 | $15.9220\pm 0.0031$ | $1.3389^{+0.1013}_{-0.1013}$ | SHC
2803 A | $2.0234\pm 0.0117$ |  $0.749\pm 0.009$ | $11.908\pm 0.011$ | 0.073 | $12.4168\pm 0.0028$ |  |
2803 B | $2.0241\pm 0.0119$ |  $0.795\pm 0.009$ | $11.972\pm 0.011$ | 0.066 | $12.7534\pm 0.0028$ | $0.0260^{+0.0950}_{-0.0220}$ |
2816 B | $1.9855\pm 0.0138$ | $18.981\pm 0.015$ |  $1.137\pm 0.016$ | 0.063 | $13.9355\pm 0.0028$ |  |
2816 A | $2.0217\pm 0.0092$ | $18.496\pm 0.009$ |  $1.112\pm 0.010$ | 0.000 | $12.6136\pm 0.0028$ | $1.6313^{+0.1550}_{-0.2834}$ |
2892 A | $2.6068\pm 0.0137$ | $-8.416\pm 0.017$ |  $6.244\pm 0.019$ | 0.009 | $13.9810\pm 0.0028$ | $0.2410^{+0.0738}_{-0.1176}$ |
2892 B | $2.7029\pm 0.0414$ | $-7.484\pm 0.058$ |  $6.334\pm 0.058$ | 0.382 | $15.1238\pm 0.0029$ |  |
2909 A | $1.8407\pm 0.1081$ | $-10.374\pm 0.097$ |  $3.687\pm 0.120$ | 1.189 | $11.5362\pm 0.0028$ | $0.8720^{+0.0700}_{-0.0951}$ |
2909 B | $1.3577\pm 0.0555$ | $-10.198\pm 0.047$ |  $3.328\pm 0.063$ | 0.547 | $14.2692\pm 0.0028$ |  |
2911 A | $5.5605\pm 0.0220$ | $-32.895\pm 0.024$ | $39.756\pm 0.025$ | 0.054 | $15.3347\pm 0.0029$ |  |
2911 B | $5.5101\pm 0.0423$ | $-33.121\pm 0.046$ | $39.720\pm 0.054$ | 0.347 | $16.1902\pm 0.0028$ | $1.1278^{+0.4704}_{-0.4704}$ | SHC
2956 A | $2.7756\pm 0.0123$ | $14.483\pm 0.014$ | $-5.685\pm 0.014$ | 0.081 | $12.9223\pm 0.0028$ | $0.0951^{+0.1019}_{-0.0951}$ | SHC
2956 B | $2.8875\pm 0.0994$ | $14.348\pm 0.120$ | $-5.420\pm 0.115$ | 0.154 | $18.1029\pm 0.0031$ |  |
3039 A | $2.2584\pm 0.0142$ | $-22.097\pm 0.017$ |  $7.596\pm 0.018$ | 0.124 | $12.9689\pm 0.0028$ | $0.3960^{+0.1411}_{-0.1140}$ |
3039 B | $2.0635\pm 0.2918$ | $-23.398\pm 0.326$ |  $4.107\pm 0.348$ | 0.856 | $19.5510\pm 0.0045$ |  |
3040 A | $2.1777\pm 0.0084$ | $-29.827\pm 0.010$ | $15.771\pm 0.010$ | 0.031 | $12.6178\pm 0.0028$ |  |
3040 B | $2.1904\pm 0.0099$ | $-29.960\pm 0.012$ | $15.665\pm 0.012$ | 0.072 | $12.7458\pm 0.0028$ | $0.2197^{+0.1653}_{-0.0822}$ |
3073 A | $16.0192\pm 0.0633$ | $-42.316\pm 0.046$ | $-82.667\pm 0.068$ | 0.566 | $12.9160\pm 0.0029$ |  |
3073 B | $16.2470\pm 0.0967$ | $-37.439\pm 0.048$ | $-87.657\pm 0.116$ | 0.474 | $13.0601\pm 0.0032$ | $0.0000^{+0.0543}_{-0.0000}$ | SHC
3097 A | $2.4078\pm 0.0184$ | $-16.449\pm 0.013$ | $25.469\pm 0.014$ | 0.068 | $13.7774\pm 0.0028$ |  |
3097 B | $2.4004\pm 0.0375$ | $-16.803\pm 0.035$ | $25.317\pm 0.040$ | 0.086 | $15.1920\pm 0.0045$ | $0.0000^{+0.3472}_{-0.0000}$ | SHC
3106 A | $2.4846\pm 0.0375$ | $-34.590\pm 0.041$ | $-6.137\pm 0.030$ | 0.283 | $12.4863\pm 0.0028$ |  |
3106 B | $2.1856\pm 0.1414$ | $-42.201\pm 0.164$ | $-5.029\pm 0.117$ | 0.303 | $18.0587\pm 0.0033$ |  |
3106 C | $2.5911\pm 0.2775$ | $-35.221\pm 0.346$ | $-6.048\pm 0.376$ | 0.502 | $18.4780\pm 0.0079$ |  |
3106 D | $2.3662\pm 0.3323$ | $-42.467\pm 0.356$ | $-5.403\pm 0.274$ | 0.525 | $19.3475\pm 0.0045$ |  |
3155 A | $4.9802\pm 0.0118$ | $-30.047\pm 0.008$ |  $2.360\pm 0.010$ | 0.054 | $12.2016\pm 0.0029$ | $0.4635^{+0.2566}_{-0.1975}$ |
3155 B | $4.9645\pm 0.0637$ | $-30.140\pm 0.047$ |  $2.263\pm 0.053$ | 0.056 | $17.0518\pm 0.0028$ |  |
3159 A | $2.3238\pm 0.0126$ | $14.274\pm 0.010$ | $-7.779\pm 0.012$ | 0.078 | $11.7695\pm 0.0028$ |  |
3159 B | $2.2756\pm 0.0596$ | $14.337\pm 0.052$ | $-7.802\pm 0.065$ | 0.194 | $16.8338\pm 0.0030$ | $1.1801^{+0.4039}_{-0.4039}$ | SHC
3179 A | $2.2367\pm 0.0192$ | $-13.150\pm 0.022$ | $16.482\pm 0.022$ | 0.184 | $12.6238\pm 0.0028$ |  |
3179 B | $2.2209\pm 0.0626$ | $-14.335\pm 0.111$ | $16.021\pm 0.045$ | 0.186 | $14.1466\pm 0.0030$ | $0.0000^{+0.4931}_{-0.0000}$ | SHC
3202 A | $2.6257\pm 0.0196$ | $-17.827\pm 0.021$ | $-10.501\pm 0.019$ | 0.125 | $12.8707\pm 0.0028$ | $0.6382^{+0.1162}_{-0.1162}$ | SHC
3202 B | $2.7703\pm 0.1460$ | $-17.690\pm 0.173$ | $-10.641\pm 0.138$ | 0.151 | $18.3475\pm 0.0032$ |  |
3205 A | $4.0476\pm 0.0440$ | $-131.821\pm 0.049$ | $-35.458\pm 0.038$ | 0.278 | $14.3176\pm 0.0028$ | $0.3053^{+0.4982}_{-0.2789}$ |
3205 B | $3.9962\pm 0.0782$ | $-130.496\pm 0.089$ | $-35.008\pm 0.067$ | 0.409 | $16.2783\pm 0.0036$ |  |
3250 A | $2.3659\pm 0.0218$ | $-27.450\pm 0.023$ |  $9.163\pm 0.021$ | 0.041 | $12.5500\pm 0.0028$ |  |
3250 B | $2.4710\pm 0.1478$ | $-27.086\pm 0.140$ |  $8.708\pm 0.147$ | 0.677 | $14.8428\pm 0.0031$ | $1.4263^{+0.3198}_{-0.4411}$ |

Table 3: continued

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
3252 A | $3.6369\pm 0.0171$ | $-47.791\pm 0.018$ | $-46.007\pm 0.019$ | 0.064 | $13.0062\pm 0.0028$ |  |
3252 B | $3.6551\pm 0.0208$ | $-47.701\pm 0.022$ | $-46.008\pm 0.024$ | 0.049 | $13.9073\pm 0.0028$ | $0.5420^{+0.3447}_{-0.1705}$ |
3266 A | $1.9643\pm 0.0269$ | $13.758\pm 0.033$ |  $4.392\pm 0.029$ | 0.295 | $12.7626\pm 0.0028$ |  |
3266 B | $1.9978\pm 0.0184$ | $13.303\pm 0.037$ |  $4.516\pm 0.028$ | 0.100 | $13.5277\pm 0.0028$ | $0.0000^{+0.4945}_{-0.0000}$ | SHC
3277 A | $3.6645\pm 0.0145$ | $36.441\pm 0.011$ | $-117.552\pm 0.010$ | 0.000 | $13.3531\pm 0.0028$ |  |
3277 B | $3.7431\pm 0.0658$ | $36.204\pm 0.050$ | $-117.525\pm 0.047$ | 0.335 | $16.2788\pm 0.0033$ | $1.7400^{+0.4530}_{-0.4530}$ | SHC
3284 A | $2.0513\pm 0.0454$ | $-2.842\pm 0.044$ |  $3.096\pm 0.035$ | 0.371 | $11.3851\pm 0.0028$ | $0.1411^{+0.1729}_{-0.1411}$ | SHC
3284 B | $2.2253\pm 0.2558$ | $-2.887\pm 0.309$ |  $2.973\pm 0.250$ | 0.659 | $18.5826\pm 0.0149$ |  |
3288 A | $4.9687\pm 0.0248$ | $-6.566\pm 0.022$ | $-20.080\pm 0.014$ | 0.041 | $14.2346\pm 0.0028$ | $1.0060^{+0.1690}_{-0.3141}$ |
3288 B | $5.3843\pm 0.1201$ | $-6.719\pm 0.114$ | $-20.952\pm 0.073$ | 0.450 | $17.2239\pm 0.0031$ |  |
3294 A | $2.8964\pm 0.0205$ |  $7.488\pm 0.017$ | $-6.949\pm 0.014$ | 0.137 | $12.2883\pm 0.0028$ | $1.0358^{+0.4293}_{-0.4805}$ |
3294 B | $3.0028\pm 0.0205$ |  $7.605\pm 0.017$ | $-7.933\pm 0.015$ | 0.132 | $12.5503\pm 0.0047$ |  |
3314 A | $1.8765\pm 0.0428$ |  $5.630\pm 0.046$ | $-4.350\pm 0.042$ | 0.309 | $13.0442\pm 0.0032$ | $0.5955^{+0.2416}_{-0.1916}$ |
3314 B | $2.0938\pm 0.0866$ |  $6.610\pm 0.098$ | $-4.803\pm 0.086$ | 0.176 | $17.1279\pm 0.0038$ |  |
3342 B | $2.9571\pm 0.0142$ | $-9.769\pm 0.013$ | $-24.855\pm 0.011$ | 0.057 | $12.3031\pm 0.0028$ |  |
3342 A | $2.8911\pm 0.0246$ | $-9.779\pm 0.022$ | $-24.778\pm 0.020$ | 0.150 | $10.9629\pm 0.0028$ | $0.3310^{+0.2686}_{-0.2071}$ |
3344 A | $4.0494\pm 0.0289$ | $-9.860\pm 0.029$ | $-3.521\pm 0.021$ | 0.077 | $11.4234\pm 0.0028$ |  |
3344 B | $4.0057\pm 0.0481$ | $-8.921\pm 0.046$ | $-3.676\pm 0.029$ | 0.117 | $14.5398\pm 0.0030$ | $0.0000^{+0.3096}_{-0.0000}$ | SHC
3353 A | $12.6836\pm 0.0105$ | $-5.941\pm 0.013$ | $38.620\pm 0.013$ | 0.059 |  $9.2522\pm 0.0034$ |  |
3353 B | $12.6756\pm 0.0319$ | $-8.591\pm 0.040$ | $38.947\pm 0.042$ | 0.171 | $15.8066\pm 0.0029$ | $0.7513^{+0.3138}_{-0.2249}$ |
3355 A | $3.7893\pm 0.0141$ | $12.255\pm 0.018$ | $37.028\pm 0.019$ | 0.100 | $11.1883\pm 0.0028$ | $0.0090^{+0.1485}_{-0.0090}$ |
3355 B | $3.4693\pm 0.0994$ | $12.573\pm 0.127$ | $37.110\pm 0.155$ | 0.441 | $16.9064\pm 0.0043$ |  |
3386 A | $1.9732\pm 0.0270$ | $-3.972\pm 0.027$ | $-0.951\pm 0.030$ | 0.283 | $12.9104\pm 0.0028$ | $0.2950^{+0.1130}_{-0.1211}$ |
3386 B | $1.5039\pm 0.3109$ | $-3.630\pm 0.280$ | $-1.099\pm 0.339$ | 0.583 | $19.5938\pm 0.0063$ |  |
3398 A | $6.0119\pm 0.0164$ | $39.572\pm 0.018$ | $-59.047\pm 0.012$ | 0.097 | $12.8762\pm 0.0028$ | $0.1690^{+0.1623}_{-0.1071}$ |
3398 B | $5.8215\pm 0.2057$ | $39.506\pm 0.227$ | $-60.221\pm 0.155$ | 0.679 | $18.9304\pm 0.0039$ |  |
3444 A | $2.0369\pm 0.0169$ | $-9.773\pm 0.017$ | $-6.666\pm 0.013$ | 0.101 | $12.4612\pm 0.0028$ | $1.0403^{+0.2006}_{-0.1879}$ |
3444 B | $1.9657\pm 0.5421$ | $-7.917\pm 0.564$ | $-6.394\pm 0.487$ | 0.474 | $20.0347\pm 0.0155$ |  |
3450 A | $3.8886\pm 0.0499$ | $-18.362\pm 0.042$ | $-14.793\pm 0.055$ | 0.356 | $11.7634\pm 0.0028$ |  |
3450 B | $3.3865\pm 0.0670$ | $-18.130\pm 0.061$ | $-16.052\pm 0.084$ | 0.514 | $11.8100\pm 0.0030$ |  |
3490 B | $3.6770\pm 0.0098$ | $-19.944\pm 0.013$ | $12.563\pm 0.011$ | 0.000 | $13.2023\pm 0.0028$ |  |
3490 A | $3.6705\pm 0.0102$ | $-19.247\pm 0.013$ | $11.830\pm 0.012$ | 0.081 | $12.0595\pm 0.0028$ | $0.3050^{+0.2115}_{-0.1521}$ |
3491 A | $1.8445\pm 0.1476$ | $-8.101\pm 0.190$ | $-14.372\pm 0.134$ | 1.257 | $12.6121\pm 0.0029$ |  |
3491 B | $1.7043\pm 0.0225$ | $-7.265\pm 0.026$ | $-14.492\pm 0.021$ | 0.000 | $14.7859\pm 0.0028$ | $0.3670^{+0.2306}_{-0.2478}$ |
3492 A | $4.9324\pm 0.0137$ | $-8.903\pm 0.016$ | $-1.924\pm 0.015$ | 0.094 | $8.8301\pm 0.028$ | $0.2360^{+0.2513}_{-0.2360}$ | SHC
3492 B | $4.0531\pm 1.2172$ | $-8.824\pm 1.703$ | $-1.747\pm 1.531$ | 2.199 | $20.7374\pm 0.0123$ |  |
3500 A | $5.1961\pm 0.0275$ | $-58.420\pm 0.028$ | $-38.469\pm 0.025$ | 0.201 | $11.3464\pm 0.0028$ | $0.3050^{+0.2660}_{-0.1344}$ |
3500 B | $5.2136\pm 0.0277$ | $-56.720\pm 0.030$ | $-39.769\pm 0.026$ | 0.158 | $14.0653\pm 0.0028$ |  |
3503 B | $2.2555\pm 0.0162$ | $-14.127\pm 0.019$ | $-1.361\pm 0.016$ | 0.145 | $10.4002\pm 0.0028$ |  |
3503 A | $2.2162\pm 0.0257$ | $-15.004\pm 0.030$ | $-1.096\pm 0.026$ | 0.270 | $9.5537\pm 0.028$ | $0.3590^{+0.0716}_{-0.1691}$ |
3504 B | $3.3547\pm 0.0116$ |  $4.594\pm 0.008$ | $-10.666\pm 0.011$ | 0.062 | $12.0330\pm 0.0031$ |  |
3504 A | $3.3862\pm 0.0127$ |  $4.657\pm 0.009$ | $-10.577\pm 0.012$ | 0.084 | $10.9256\pm 0.0028$ | $0.7582^{+0.4521}_{-0.3753}$ |
3514 A | $2.3913\pm 0.0117$ |  $5.950\pm 0.011$ | $13.680\pm 0.012$ | 0.000 | $13.4043\pm 0.0028$ | $0.1790^{+0.2678}_{-0.1314}$ |
3514 B | $2.4018\pm 0.0632$ |  $5.398\pm 0.058$ | $13.328\pm 0.077$ | 0.416 | $16.4625\pm 0.0032$ |  |
3522 A | $2.6061\pm 0.0112$ | $-5.315\pm 0.011$ | $-6.051\pm 0.012$ | 0.000 | $13.4646\pm 0.0028$ |  |
3522 B | $2.6225\pm 0.0139$ | $-5.170\pm 0.014$ | $-5.927\pm 0.015$ | 0.000 | $14.1333\pm 0.0028$ | $0.3870^{+0.1843}_{-0.1831}$ |
3531 A | $2.7694\pm 0.0132$ | $-17.657\pm 0.016$ | $-15.849\pm 0.014$ | 0.124 | $11.0653\pm 0.0028$ | $0.8130^{+0.1943}_{-0.2726}$ |
3531 B | $2.4929\pm 0.4232$ | $-17.963\pm 0.553$ | $-15.183\pm 0.610$ | 1.330 | $19.8962\pm 0.0117$ |  |

Table 3: continued

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
3533 B | $4.1368\pm 0.8172$ | $-3.067\pm 0.773$ | $-13.748\pm 0.805$ | 8.599 | $12.5867\pm 0.0081$ |  |
3533 A | $2.3155\pm 0.0105$ | $-7.333\pm 0.010$ | $-13.811\pm 0.011$ | 0.050 | $12.3977\pm 0.0028$ | $0.4550^{+0.1468}_{-0.2494}$ |
3560 A | $3.2964\pm 0.0153$ |  $6.494\pm 0.016$ |  $1.589\pm 0.019$ | 0.152 | $11.1630\pm 0.0028$ | $0.2150^{+0.1330}_{-0.0935}$ |
3560 B | $3.5079\pm 0.1034$ |  $6.785\pm 0.113$ |  $0.342\pm 0.137$ | 1.166 | $14.3548\pm 0.0028$ |  |
3584 A | $2.2622\pm 0.0278$ | $16.974\pm 0.037$ |  $9.218\pm 0.033$ | 0.323 | $12.9741\pm 0.0028$ |  |
3584 B | $2.2790\pm 0.0230$ | $17.235\pm 0.048$ |  $8.602\pm 0.019$ | 0.098 | $13.5272\pm 0.0028$ | $0.0000^{+0.5098}_{-0.0000}$ | SHC
3584 C | $2.2733\pm 0.0511$ | $17.298\pm 0.063$ |  $8.818\pm 0.058$ | 0.000 | $17.0914\pm 0.0028$ | $0.3311^{+0.2004}_{-0.2004}$ | SHC
3586 A | $4.2460\pm 0.0252$ | $-7.353\pm 0.029$ | $15.291\pm 0.029$ | 0.266 | $12.9751\pm 0.0028$ | $0.0213^{+0.1764}_{-0.0093}$ |
3586 B | $4.3772\pm 0.1051$ | $-6.617\pm 0.116$ | $15.471\pm 0.137$ | 0.407 | $17.9469\pm 0.0035$ |  |
3607 A | $1.9354\pm 0.0333$ |  $8.910\pm 0.050$ | $-11.664\pm 0.041$ | 0.336 | $14.0234\pm 0.0029$ |  |
3607 B | $1.8921\pm 0.0368$ |  $8.962\pm 0.095$ | $-10.626\pm 0.075$ | 0.209 | $15.0427\pm 0.0028$ | $0.0000^{+0.4805}_{-0.0000}$ | SHC
3628 A | $2.9968\pm 0.0132$ | $37.585\pm 0.014$ | $-12.397\pm 0.011$ | 0.075 | $12.0879\pm 0.0028$ | $0.3150^{+0.1870}_{-0.1306}$ |
3628 B | $2.9882\pm 0.0125$ | $37.716\pm 0.013$ | $-12.074\pm 0.011$ | 0.061 | $12.2215\pm 0.0028$ |  |
3628 C | $3.0086\pm 0.1063$ | $37.078\pm 0.089$ | $-14.423\pm 0.338$ | 0.388 | $16.0404\pm 0.0034$ |  |
3634 A | $2.0145\pm 0.2116$ | $-8.268\pm 0.203$ | $-4.232\pm 0.122$ | 1.370 | $12.1373\pm 0.0032$ |  |
3634 B | $2.4055\pm 0.3678$ | $-6.206\pm 0.418$ | $-4.784\pm 0.160$ | 1.533 | $12.5085\pm 0.0033$ |  |
3636 A | $2.2499\pm 0.0166$ | $-9.242\pm 0.015$ | $-16.771\pm 0.016$ | 0.005 | $13.2711\pm 0.0028$ | $0.3300^{+0.1700}_{-0.1861}$ |
3636 B | $5.7508\pm 0.9837$ | $-7.768\pm 0.986$ | $-15.159\pm 0.598$ | 1.432 | $19.3550\pm 0.0157$ |  |
3642 A | $2.7064\pm 0.0165$ | $10.396\pm 0.015$ | $-10.158\pm 0.014$ | 0.000 | $13.0922\pm 0.0028$ | $0.2423^{+0.1607}_{-0.1641}$ |
3642 B | $2.4452\pm 0.1005$ |  $9.815\pm 0.100$ | $-10.694\pm 0.094$ | 0.302 | $16.9979\pm 0.0031$ |  |
3682 A | $2.5213\pm 0.0170$ | $34.818\pm 0.023$ | $-18.553\pm 0.015$ | 0.070 | $11.8685\pm 0.0028$ |  |
3682 B | $2.2612\pm 0.0533$ | $35.839\pm 0.068$ | $-13.332\pm 0.044$ | 0.000 | $15.9081\pm 0.0028$ | $0.3303^{+0.3697}_{-0.2119}$ |
3688 A | $2.5118\pm 0.0111$ | $18.777\pm 0.009$ | $-11.398\pm 0.013$ | 0.014 | $12.3571\pm 0.0028$ | $0.7613^{+0.2787}_{-0.2634}$ |
3688 B | $2.5109\pm 0.1834$ | $18.860\pm 0.168$ | $-11.127\pm 0.246$ | 0.549 | $18.4505\pm 0.0042$ |  |
3712 A | $2.8275\pm 0.0249$ | $13.023\pm 0.023$ | $-15.880\pm 0.016$ | 0.082 | $14.1183\pm 0.0028$ |  |
3712 B | $3.0133\pm 0.1160$ | $13.093\pm 0.106$ | $-15.686\pm 0.077$ | 0.000 | $17.5023\pm 0.0030$ | $0.2394^{+0.0189}_{-0.0189}$ | SHC
3714 A | $8.8385\pm 0.0219$ | $19.826\pm 0.025$ | $-70.762\pm 0.020$ | 0.057 | $14.2908\pm 0.0028$ | $0.4560^{+0.4346}_{-0.1474}$ |
3714 B | $8.8470\pm 0.2265$ | $18.805\pm 0.252$ | $-70.672\pm 0.205$ | 0.190 | $18.8475\pm 0.0034$ |  |
3724 A | $2.2760\pm 0.0150$ |  $6.687\pm 0.017$ | $-18.321\pm 0.012$ | 0.054 | $12.1368\pm 0.0028$ | $0.5900^{+0.1610}_{-0.1327}$ |
3724 B | $1.6154\pm 0.3318$ |  $6.398\pm 0.437$ | $-17.956\pm 0.305$ | 0.871 | $18.2689\pm 0.0087$ |  |
3741 A | $2.0778\pm 0.2075$ | $-0.899\pm 0.236$ | $-0.564\pm 0.182$ | 1.673 | $13.7007\pm 0.0035$ | $0.5460^{+0.3191}_{-0.3610}$ |
3741 B | $1.3246\pm 0.0324$ | $-0.592\pm 0.036$ | $-1.069\pm 0.031$ | 0.168 | $14.6383\pm 0.0041$ |  |
3742 B | $5.9961\pm 0.0168$ | $40.533\pm 0.021$ | $-29.932\pm 0.018$ | 0.000 | $13.8193\pm 0.0028$ | $0.9093^{+0.2657}_{-0.4189}$ |
3742 A | $5.9830\pm 0.0150$ | $40.490\pm 0.018$ | $-30.866\pm 0.016$ | 0.062 | $12.9491\pm 0.0028$ |  |
3745 A | $2.8689\pm 0.0252$ |  $6.312\pm 0.025$ | $-19.652\pm 0.017$ | 0.094 | $13.8210\pm 0.0028$ |  |
3745 B | $2.8982\pm 0.0271$ |  $5.432\pm 0.027$ | $-19.348\pm 0.022$ | 0.107 | $13.8686\pm 0.0028$ | $0.6417^{+0.2931}_{-0.3698}$ |
3758 A | $1.9972\pm 0.0144$ |  $0.312\pm 0.011$ | $-6.801\pm 0.014$ | 0.080 | $13.2349\pm 0.0028$ | $1.6340^{+0.4285}_{-0.4891}$ |
3758 B | $1.9234\pm 0.0977$ |  $1.280\pm 0.121$ | $-7.528\pm 0.119$ | 0.412 | $16.5664\pm 0.0034$ |  |
3761 B | $4.5911\pm 0.0126$ | $17.162\pm 0.008$ | $-26.434\pm 0.012$ | 0.000 | $13.5745\pm 0.0028$ |  |
3761 A | $4.6027\pm 0.0098$ | $16.199\pm 0.006$ | $-25.933\pm 0.009$ | 0.041 | $12.2262\pm 0.0028$ | $0.2090^{+0.1011}_{-0.0840}$ |
3781 A | $3.6818\pm 0.0157$ | $-11.557\pm 0.015$ | $-22.175\pm 0.012$ | 0.100 | $12.9944\pm 0.0028$ |  |
3781 B | $3.6742\pm 0.0330$ | $-12.882\pm 0.033$ | $-22.261\pm 0.025$ | 0.091 | $15.6283\pm 0.0028$ | $0.4810^{+0.5230}_{-0.0961}$ |
3791 A | $2.0635\pm 0.0089$ | $-4.514\pm 0.011$ | $-14.888\pm 0.013$ | 0.071 | $11.9164\pm 0.0028$ |  |
3791 B | $2.0890\pm 0.0091$ | $-4.510\pm 0.011$ | $-14.938\pm 0.012$ | 0.066 | $12.4252\pm 0.0028$ | $0.2803^{+0.0887}_{-0.1663}$ |
3795 A | $2.2947\pm 0.0164$ | $-1.150\pm 0.015$ | $-1.011\pm 0.014$ | 0.090 | $12.6766\pm 0.0029$ |  |
3795 B | $2.3590\pm 0.0670$ | $-0.959\pm 0.057$ | $-0.886\pm 0.055$ | 0.212 | $16.6713\pm 0.0029$ | $0.0377^{+0.1564}_{-0.0307}$ |

Table 3: continued

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
3797 A | $2.4942\pm 0.0148$ | $-7.945\pm 0.015$ | $-6.929\pm 0.013$ | 0.066 | $12.2200\pm 0.0028$ |  |
3797 B | $2.4782\pm 0.0263$ | $-8.278\pm 0.028$ | $-7.068\pm 0.025$ | 0.000 | $14.7839\pm 0.0028$ | $0.2037^{+0.3781}_{-0.1488}$ |
3801 A | $2.0122\pm 0.0149$ | $-5.623\pm 0.014$ | $-14.080\pm 0.010$ | 0.000 | $13.4814\pm 0.0028$ | $0.6540^{+0.1331}_{-0.2991}$ |
3801 B | $1.8222\pm 0.2313$ | $-5.501\pm 0.213$ | $-13.954\pm 0.164$ | 0.646 | $18.7086\pm 0.0070$ |  |
3823 A | $2.2333\pm 0.0553$ | $-10.275\pm 0.051$ | $-11.383\pm 0.054$ | 0.449 | $11.8176\pm 0.0028$ | $0.1570^{+0.1190}_{-0.1481}$ |
3823 B | $2.6615\pm 0.2345$ | $-9.984\pm 0.213$ | $-10.688\pm 0.201$ | 0.918 | $18.0512\pm 0.0093$ |  |
3828 A | $2.8895\pm 0.0136$ | $-11.854\pm 0.012$ | $-36.352\pm 0.014$ | 0.111 | $11.7578\pm 0.0028$ | $0.9041^{+0.2465}_{-0.2465}$ | SHC
3828 B | $2.9390\pm 0.0139$ | $-11.521\pm 0.013$ | $-35.619\pm 0.014$ | 0.114 | $11.9981\pm 0.0028$ |  |
3829 A | $2.5534\pm 0.0299$ |  $7.929\pm 0.027$ | $-22.846\pm 0.027$ | 0.128 | $12.8680\pm 0.0028$ | $0.5270^{+0.2186}_{-0.2884}$ |
3829 B | $2.2647\pm 0.0746$ |  $6.321\pm 0.100$ | $-20.316\pm 0.115$ | 0.229 | $14.5632\pm 0.0147$ |  |
3867 A | $2.0764\pm 0.0142$ | $-30.294\pm 0.011$ | $-8.137\pm 0.012$ | 0.088 | $13.2021\pm 0.0028$ | $0.4130^{+0.1199}_{-0.2401}$ |
3867 B | $1.9565\pm 0.2303$ | $-30.050\pm 0.231$ | $-8.052\pm 0.191$ | 1.041 | $18.9153\pm 0.0062$ |  |
3872 A | $2.5321\pm 0.0167$ | $12.211\pm 0.015$ | $-27.290\pm 0.014$ | 0.080 | $12.8266\pm 0.0028$ |  |
3872 B | $2.5096\pm 0.0565$ | $11.765\pm 0.050$ | $-27.605\pm 0.048$ | 0.423 | $14.5556\pm 0.0028$ | $0.2173^{+0.3142}_{-0.2093}$ |
3875 A | $2.5131\pm 0.0111$ |  $6.276\pm 0.014$ | $-23.960\pm 0.013$ | 0.058 | $12.4824\pm 0.0028$ |  |
3875 B | $2.3635\pm 0.0392$ |  $6.079\pm 0.046$ | $-23.853\pm 0.043$ | 0.377 | $14.4436\pm 0.0028$ | $0.8483^{+0.2928}_{-0.4564}$ |
3883 A | $2.0150\pm 0.0145$ | $-11.230\pm 0.007$ | $-3.464\pm 0.011$ | 0.086 | $12.2750\pm 0.0028$ | $0.5400^{+0.2986}_{-0.4084}$ |
3883 B | $2.0994\pm 0.0864$ | $-11.426\pm 0.040$ | $-3.610\pm 0.061$ | 0.380 | $17.1427\pm 0.0029$ |  |
3889 A | $3.2539\pm 0.0139$ | $-28.881\pm 0.013$ | $-36.522\pm 0.016$ | 0.075 | $12.9323\pm 0.0028$ |  |
3889 B | $3.2854\pm 0.0295$ | $-27.235\pm 0.027$ | $-35.533\pm 0.033$ | 0.147 | $15.1588\pm 0.0028$ | $0.6490^{+0.5260}_{-0.4961}$ |
3896 A | $5.4600\pm 0.0098$ | $-108.453\pm 0.011$ | $-4.958\pm 0.010$ | 0.055 | $12.2257\pm 0.0028$ |  |
3896 B | $5.5026\pm 0.0296$ | $-108.505\pm 0.034$ | $-5.017\pm 0.031$ | 0.091 | $15.8077\pm 0.0028$ | $0.3085^{+0.1855}_{-0.1346}$ |
3915 A | $3.5926\pm 0.0159$ | $-36.921\pm 0.015$ | $35.332\pm 0.011$ | 0.080 | $12.8996\pm 0.0028$ | $0.1602^{+0.0479}_{-0.0170}$ |
3915 B | $3.6064\pm 0.1920$ | $-38.018\pm 0.161$ | $36.095\pm 0.136$ | 0.790 | $17.3797\pm 0.0062$ |  |
3920 A | $2.0001\pm 0.0116$ | $10.234\pm 0.012$ |  $6.142\pm 0.011$ | 0.000 | $13.3445\pm 0.0028$ | $0.9260^{+0.2461}_{-0.3135}$ |
3920 B | $1.9917\pm 0.0282$ | $10.392\pm 0.031$ |  $6.171\pm 0.027$ | 0.127 | $15.3209\pm 0.0028$ |  |
3922 B | $3.7843\pm 0.0168$ | $40.170\pm 0.013$ | $-35.715\pm 0.020$ | 0.139 | $12.7800\pm 0.0028$ |  |
3922 A | $3.7885\pm 0.0122$ | $39.376\pm 0.010$ | $-35.779\pm 0.014$ | 0.088 | $12.3127\pm 0.0028$ | $0.1977^{+0.0914}_{-0.0923}$ |
3956 B | $2.3213\pm 0.0129$ | $-9.642\pm 0.013$ | $-0.124\pm 0.015$ | 0.039 | $13.6040\pm 0.0028$ |  |
3956 A | $2.3444\pm 0.0255$ | $-9.131\pm 0.025$ | $-1.189\pm 0.030$ | 0.258 | $12.5291\pm 0.0028$ | $0.5955^{+0.2416}_{-0.1420}$ |
3966 A | $3.3953\pm 0.2509$ | $-3.736\pm 0.201$ | $-18.230\pm 0.233$ | 2.597 | $12.6688\pm 0.0034$ | $0.0347^{+0.1524}_{-0.0248}$ |
3966 B | $2.8621\pm 0.0911$ | $-3.562\pm 0.071$ | $-19.212\pm 0.086$ | 0.476 | $17.4805\pm 0.0051$ |  |
3977 A | $4.4761\pm 0.0093$ | $19.633\pm 0.010$ | $-59.020\pm 0.012$ | 0.057 | $11.8382\pm 0.0028$ |  |
3977 B | $4.4895\pm 0.0114$ | $19.414\pm 0.012$ | $-58.492\pm 0.017$ | 0.052 | $13.1923\pm 0.0028$ | $0.2340^{+0.3740}_{-0.1737}$ |
3984 A | $9.1843\pm 0.0191$ | $-48.951\pm 0.016$ | $42.647\pm 0.020$ | 0.056 | $14.6487\pm 0.0028$ | $0.2210^{+0.1528}_{-0.1528}$ | SHC
3984 B | $9.0569\pm 0.2022$ | $-50.379\pm 0.163$ | $40.950\pm 0.212$ | 0.000 | $19.0813\pm 0.0035$ |  |
3998 A | $2.4433\pm 0.0109$ | $40.382\pm 0.008$ | $-4.035\pm 0.011$ | 0.025 | $12.5908\pm 0.0028$ |  |
3998 B | $2.3977\pm 0.0519$ | $40.274\pm 0.041$ | $-3.563\pm 0.049$ | 0.237 | $16.4309\pm 0.0036$ | $0.0000^{+0.2236}_{-0.0000}$ | SHC
4001 A | $3.1839\pm 0.0099$ | $38.437\pm 0.010$ | $-7.216\pm 0.010$ | 0.036 | $12.1892\pm 0.0028$ |  |
4001 B | $3.1813\pm 0.0149$ | $38.834\pm 0.016$ | $-7.364\pm 0.015$ | 0.000 | $14.0300\pm 0.0028$ | $0.3650^{+0.1870}_{-0.0320}$ |
4021 A | $2.0152\pm 0.0150$ | $13.008\pm 0.012$ | $-4.221\pm 0.013$ | 0.124 | $11.5185\pm 0.0028$ |  |
4021 B | $2.0244\pm 0.0226$ | $12.367\pm 0.018$ | $-4.988\pm 0.019$ | 0.000 | $15.1104\pm 0.0028$ | $0.5990^{+0.2425}_{-0.2863}$ |
4040 A | $3.3950\pm 0.0120$ | $-0.367\pm 0.015$ | $18.861\pm 0.017$ | 0.084 | $12.8525\pm 0.0028$ | $0.0795^{+0.1465}_{-0.0608}$ |
4040 B | $5.1879\pm 0.9560$ | $-2.278\pm 1.485$ | $14.109\pm 2.231$ | 2.820 | $20.4319\pm 0.0107$ |  |
4059 A | $2.9516\pm 0.0118$ |  $4.954\pm 0.015$ | $25.093\pm 0.017$ | 0.053 | $13.6797\pm 0.0028$ | $0.2560^{+0.1831}_{-0.1080}$ |
4059 B | $2.7338\pm 0.1000$ |  $4.172\pm 0.137$ | $25.217\pm 0.145$ | 0.554 | $17.8747\pm 0.0032$ |  |

Table 3: continued

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
4070 B | $2.4449\pm 0.0122$ |  $8.642\pm 0.013$ | $-18.269\pm 0.016$ | 0.080 | $13.5274\pm 0.0028$ |  |
4070 A | $2.6418\pm 0.0200$ |  $9.336\pm 0.021$ | $-18.455\pm 0.026$ | 0.230 | $12.5658\pm 0.0028$ | $0.3410^{+0.1836}_{-0.0680}$ |
4077 A | $3.2950\pm 0.0105$ | $14.495\pm 0.010$ | $-5.085\pm 0.014$ | 0.000 | $13.4583\pm 0.0028$ | $0.2777^{+0.1923}_{-0.1073}$ |
4077 B | $3.2764\pm 0.0885$ | $14.505\pm 0.089$ | $-4.694\pm 0.108$ | 0.000 | $18.0035\pm 0.0030$ |  |
4079 B | $2.7511\pm 0.0110$ | $17.947\pm 0.008$ |  $0.738\pm 0.011$ | 0.041 | $12.6781\pm 0.0028$ |  |
4079 A | $2.7324\pm 0.0105$ | $18.083\pm 0.008$ |  $0.480\pm 0.011$ | 0.053 | $11.9719\pm 0.0028$ | $0.6147^{+0.1797}_{-0.1797}$ | SHC
4081 A | $2.2178\pm 0.0171$ | $14.352\pm 0.014$ | $-11.890\pm 0.016$ | 0.133 | $11.1647\pm 0.0028$ | $1.0309^{+0.3428}_{-0.3428}$ | SHC
4081 B | $2.2822\pm 0.0283$ | $14.464\pm 0.021$ | $-11.131\pm 0.029$ | 0.165 | $14.4743\pm 0.0028$ |  |
4089 A | $2.7202\pm 0.0160$ | $-19.332\pm 0.011$ | $-22.925\pm 0.016$ | 0.140 | $12.1023\pm 0.0028$ |  |
4089 B | $2.6560\pm 0.0319$ | $-18.932\pm 0.021$ | $-23.408\pm 0.045$ | 0.171 | $13.5114\pm 0.0028$ | $0.0000^{+0.5071}_{-0.0000}$ | SHC
4107 A | $6.5079\pm 0.0112$ | $-13.776\pm 0.012$ |  $6.051\pm 0.014$ | 0.000 | $13.6674\pm 0.0028$ | $0.2500^{+0.3414}_{-0.1203}$ |
4107 B | $6.5573\pm 0.0312$ | $-13.514\pm 0.041$ |  $6.105\pm 0.038$ | 0.274 | $15.0644\pm 0.0028$ |  |
4113 A | $6.6975\pm 0.0115$ | $12.050\pm 0.016$ | $66.562\pm 0.014$ | 0.089 | $11.6446\pm 0.0028$ | $0.0163^{+0.2653}_{-0.0083}$ |
4113 B | $6.9631\pm 0.0811$ | $12.033\pm 0.121$ | $65.993\pm 0.111$ | 0.316 | $17.4228\pm 0.0066$ |  |
4123 A | $4.1430\pm 0.0103$ | $-20.389\pm 0.009$ | $-44.515\pm 0.010$ | 0.040 | $12.3508\pm 0.0028$ | $0.1300^{+0.0777}_{-0.0595}$ |
4123 B | $4.3245\pm 0.1500$ | $-19.309\pm 0.140$ | $-44.204\pm 0.151$ | 0.747 | $17.9385\pm 0.0072$ |  |
4128 A | $3.2290\pm 0.0136$ | $-13.190\pm 0.017$ | $-28.915\pm 0.014$ | 0.086 | $12.7967\pm 0.0028$ |  |
4128 B | $3.2503\pm 0.0891$ | $-13.814\pm 0.116$ | $-28.874\pm 0.098$ | 0.894 | $13.7339\pm 0.0028$ | $0.6790^{+0.2091}_{-0.1863}$ |
4145 A | $4.9017\pm 0.0096$ | $11.694\pm 0.010$ | $-13.534\pm 0.011$ | 0.041 | $12.0492\pm 0.0028$ | $0.0890^{+0.1631}_{-0.0890}$ |
4145 B | $5.7061\pm 0.1635$ | $11.927\pm 0.199$ | $-16.830\pm 0.588$ | 0.663 | $17.3670\pm 0.0046$ |  |
4168 A | $3.0551\pm 0.0147$ | $26.083\pm 0.020$ |  $7.243\pm 0.017$ | 0.115 | $11.8651\pm 0.0028$ | $0.2373^{+0.2120}_{-0.1244}$ |
4168 B | $3.1226\pm 0.0175$ | $26.426\pm 0.024$ |  $7.408\pm 0.020$ | 0.000 | $14.5282\pm 0.0028$ |  |
4175 A | $21.5872\pm 0.0359$ | $140.238\pm 0.038$ | $-140.048\pm 0.027$ | 0.168 |  $8.6339\pm 0.0028$ |  |
4175 B | $21.8129\pm 0.0399$ | $130.361\pm 0.041$ | $-143.004\pm 0.041$ | 0.168 |  $8.8183\pm 0.0029$ | $0.9002^{+0.2040}_{-0.2040}$ | SHC
4175 C | $21.6547\pm 0.0265$ | $135.757\pm 0.031$ | $-139.611\pm 0.018$ | 0.094 | $13.7833\pm 0.0028$ | $0.0537^{+0.2814}_{-0.0403}$ |
4176 A | $2.5915\pm 0.0225$ | $-7.645\pm 0.025$ |  $8.934\pm 0.020$ | 0.124 |  $9.7568\pm 0.0028$ |  |
4176 B | $2.5938\pm 0.0237$ | $-7.619\pm 0.025$ |  $8.726\pm 0.022$ | 0.035 | $14.2051\pm 0.0028$ | $0.1095^{+0.1866}_{-0.0216}$ |
4179 B | $10.5358\pm 0.3143$ | $-60.630\pm 0.353$ |  $3.599\pm 0.223$ | 2.250 | $11.0571\pm 0.0030$ |  |
4179 A | $9.9729\pm 0.0183$ | $-63.043\pm 0.019$ |  $9.244\pm 0.014$ | 0.080 |  $9.9922\pm 0.0028$ | $0.0537^{+0.1943}_{-0.0367}$ |
4182 A | $7.5383\pm 0.0165$ | $127.765\pm 0.019$ | $58.312\pm 0.020$ | 0.169 |  $9.7074\pm 0.0028$ |  |
4182 B | $7.5374\pm 0.0391$ | $128.255\pm 0.045$ | $59.187\pm 0.051$ | 0.000 | $16.5349\pm 0.0029$ | $0.0088^{+0.1827}_{-0.0088}$ |
4192 A | $2.0501\pm 0.0120$ | $16.564\pm 0.008$ | $21.665\pm 0.010$ | 0.075 | $12.2157\pm 0.0028$ |  |
4192 B | $2.0106\pm 0.0173$ | $16.467\pm 0.011$ | $21.742\pm 0.014$ | 0.035 | $14.2976\pm 0.0029$ | $0.1340^{+0.1190}_{-0.1287}$ |
4212 A | $3.7286\pm 0.3262$ | $-2.836\pm 0.250$ |  $4.960\pm 0.322$ | 3.789 | $12.2259\pm 0.0034$ | $0.5204^{+0.2509}_{-0.2509}$ | SHC
4212 B | $7.9975\pm 1.4534$ | $-2.986\pm 0.936$ |  $3.312\pm 1.807$ | 11.289 | $20.3781\pm 0.0128$ |  |
4226 A | $2.5248\pm 0.4279$ | $-2.122\pm 0.251$ | $-0.653\pm 0.386$ | 3.553 | $11.6758\pm 0.0028$ | $0.2391^{+0.2679}_{-0.2391}$ | SHC
4226 B | $1.9440\pm 0.3435$ | $-2.352\pm 0.262$ | $-1.610\pm 0.284$ | 1.423 | $19.3122\pm 0.0064$ |  |
4245 A | $4.7788\pm 0.0124$ | $-17.313\pm 0.014$ | $28.297\pm 0.015$ | 0.106 | $12.2963\pm 0.0028$ | $0.2000^{+0.2976}_{-0.1546}$ |
4245 B | $4.8973\pm 0.1200$ | $-15.771\pm 0.157$ | $28.031\pm 0.130$ | 1.256 | $15.6363\pm 0.0037$ |  |
4293 A | $2.1309\pm 0.0145$ |  $4.296\pm 0.015$ | $-28.982\pm 0.014$ | 0.000 | $13.0778\pm 0.0028$ | $0.2693^{+0.1750}_{-0.1086}$ |
4293 B | $1.9447\pm 0.1581$ |  $3.836\pm 0.147$ | $-28.828\pm 0.148$ | 0.279 | $18.0305\pm 0.0044$ |  |
4301 A | $6.9832\pm 0.0111$ | $-64.472\pm 0.009$ | $19.070\pm 0.010$ | 0.049 | $10.6339\pm 0.0028$ | $0.1005^{+0.0936}_{-0.0775}$ |
4301 B | $6.7317\pm 0.2746$ | $-64.162\pm 0.222$ | $19.417\pm 0.351$ | 0 | $19.0917\pm 0.0037$ |  |
4303 A | $3.9464\pm 0.0121$ | $45.870\pm 0.013$ |  $0.569\pm 0.015$ | 0.104 |  $9.7193\pm 0.0028$ |  |
4303 B | $3.8848\pm 0.0204$ | $45.560\pm 0.022$ |  $0.944\pm 0.025$ | 0.106 | $14.9661\pm 0.0028$ | $0.3918^{+0.3132}_{-0.1708}$ |
4325 A | $19.5256\pm 0.0208$ | $74.703\pm 0.022$ | $-169.873\pm 0.020$ | 0.128 | $12.9796\pm 0.0028$ |  |
4325 B | $19.5097\pm 0.0378$ | $74.782\pm 0.040$ | $-170.674\pm 0.036$ | 0.125 | $15.4419\pm 0.0029$ | $0.2645^{+0.1995}_{-0.2515}$ |
4330 A | $3.4820\pm 0.0210$ | $-35.232\pm 0.023$ | $-22.466\pm 0.018$ | 0.089 |  $8.2898\pm 0.0028$ |  |
4330 B | $3.3770\pm 0.1446$ | $-35.685\pm 0.147$ | $-22.509\pm 0.117$ | 0.958 | $10.7925\pm 0.0030$ | $0.0000^{+0.2837}_{-0.0000}$ | SHC

Table 3: continued

TOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
4337 B | $15.3941\pm 0.0125$ | $-29.822\pm 0.016$ |  $0.137\pm 0.014$ | 0.073 | $12.0277\pm 0.0028$ |  |
4337 A | $15.4256\pm 0.0136$ | $-29.475\pm 0.017$ |  $0.586\pm 0.015$ | 0.083 |  $9.1343\pm 0.0028$ | $0.1440^{+0.1710}_{-0.0593}$ |
4339 B | $8.0854\pm 0.0344$ | $-79.059\pm 0.038$ | $23.767\pm 0.034$ | 0.067 | $15.2500\pm 0.0028$ |  |
4339 A | $8.1133\pm 0.0203$ | $-78.605\pm 0.022$ | $24.739\pm 0.020$ | 0.000 | $14.1382\pm 0.0031$ | $0.2660^{+0.3510}_{-0.1583}$ |
4344 A | $4.3265\pm 0.0129$ |  $8.678\pm 0.019$ | $-20.432\pm 0.017$ | 0.113 |  $9.9133\pm 0.0028$ |  |
4344 B | $4.2397\pm 0.0716$ |  $7.363\pm 0.117$ | $-21.688\pm 0.110$ | 0.604 | $15.5925\pm 0.0033$ | $0.0000^{+0.1683}_{-0.0000}$ | SHC
4349 A | $13.8901\pm 0.0209$ | $278.224\pm 0.019$ | $105.497\pm 0.018$ | 0.144 | $12.6615\pm 0.0028$ | $0.6280^{+0.2918}_{-0.2650}$ |
4349 B | $13.8550\pm 0.1123$ | $280.632\pm 0.098$ | $108.145\pm 0.090$ | 0.825 | $15.7032\pm 0.0031$ |  |
4350 A | $9.6729\pm 0.0104$ | $60.757\pm 0.014$ | $32.809\pm 0.013$ | 0.068 |  $9.3749\pm 0.0028$ | $0.1990^{+0.1670}_{-0.1051}$ |
4350 B | $9.8182\pm 0.0783$ | $59.892\pm 0.135$ | $32.989\pm 0.105$ | 0.557 | $16.2487\pm 0.0067$ |  |
4359 A | $5.6784\pm 0.0133$ | $-31.415\pm 0.014$ |  $7.856\pm 0.013$ | 0.064 |  $9.8537\pm 0.0028$ |  |
4359 B | $5.6001\pm 0.0350$ | $-32.032\pm 0.037$ |  $8.286\pm 0.038$ | 0.000 | $15.8062\pm 0.0028$ | $0.3085^{+0.1581}_{-0.1346}$ |
4366 A | $3.9742\pm 0.0114$ |  $3.884\pm 0.011$ |  $8.440\pm 0.013$ | 0.056 | $10.6782\pm 0.0028$ | $1.7163^{+0.3779}_{-0.4574}$ |
4366 B | $3.9719\pm 0.0250$ |  $4.460\pm 0.025$ |  $8.453\pm 0.031$ | 0.000 | $15.4737\pm 0.0028$ |  |
4369 A | $3.5212\pm 0.0707$ | $19.215\pm 0.086$ | $-30.255\pm 0.103$ | 0.898 |  $9.6646\pm 0.0028$ |  |
4369 B | $3.9721\pm 0.0108$ | $19.750\pm 0.013$ | $-29.086\pm 0.015$ | 0.094 | $10.0921\pm 0.0028$ | $0.1577^{+0.1633}_{-0.1577}$ | SHC
4370 A | $4.6221\pm 0.0228$ | $10.196\pm 0.024$ | $-17.865\pm 0.017$ | 0.126 |  $9.7265\pm 0.0028$ |  |
4370 B | $4.6662\pm 0.0737$ |  $9.120\pm 0.084$ | $-17.807\pm 0.052$ | 0.123 | $16.7804\pm 0.0029$ | $0.0470^{+0.0485}_{-0.0200}$ |
4372 A | $5.5395\pm 0.0924$ | $-34.738\pm 0.096$ | $-1.817\pm 0.111$ | 1.076 | $10.9396\pm 0.0029$ | $0.4855^{+0.2555}_{-0.1292}$ |
4372 B | $4.4002\pm 0.2861$ | $-35.293\pm 0.365$ |  $0.883\pm 0.347$ | 0.764 | $19.0876\pm 0.0056$ |  |
4390 A | $5.2425\pm 0.0297$ |  $2.629\pm 0.032$ | $-16.757\pm 0.023$ | 0.184 |  $9.9879\pm 0.0028$ | $1.0367^{+0.1785}_{-0.1785}$ | SHC
4390 B | $5.2339\pm 0.0345$ |  $4.544\pm 0.048$ | $-16.374\pm 0.043$ | 0.177 | $10.7970\pm 0.0031$ |  |
4414 B | $3.0877\pm 0.0483$ |  $7.006\pm 0.119$ | $-9.873\pm 0.093$ | 0.182 | $10.9572\pm 0.0048$ |  |
4414 A | $2.9238\pm 0.0388$ |  $7.477\pm 0.047$ | $-11.069\pm 0.027$ | 0.223 |  $9.7974\pm 0.0028$ |  |
4420 A | $4.3436\pm 0.0153$ |  $4.434\pm 0.011$ | $13.946\pm 0.015$ | 0.120 |  $9.9512\pm 0.0028$ |  |
4420 B | $4.3890\pm 0.0238$ |  $4.405\pm 0.021$ | $14.824\pm 0.021$ | 0.195 | $13.1066\pm 0.0028$ | $0.6837^{+0.1444}_{-0.1797}$ |
4425 A | $5.6925\pm 0.0172$ |  $1.971\pm 0.019$ | $-19.267\pm 0.013$ | 0.019 |  $9.7596\pm 0.0028$ | $0.4535^{+0.2353}_{-0.2038}$ |
4425 B | $5.6703\pm 0.0514$ |  $1.793\pm 0.054$ | $-19.380\pm 0.040$ | 0.252 | $15.4223\pm 0.0031$ |  |
4463 A | $5.6588\pm 0.0175$ | $-5.157\pm 0.017$ | $50.619\pm 0.017$ | 0.114 | $10.9509\pm 0.0028$ |  |
4463 B | $5.6443\pm 0.0673$ | $-5.258\pm 0.068$ | $50.977\pm 0.072$ | 0.154 | $16.7682\pm 0.0028$ | $0.2078^{+0.2088}_{-0.1911}$ |
4499 A | $5.6756\pm 0.0112$ | $22.425\pm 0.012$ | $29.132\pm 0.012$ | 0.083 | $10.5265\pm 0.0028$ | $0.1210^{+0.0916}_{-0.0758}$ |
4499 B | $5.6949\pm 0.0712$ | $22.160\pm 0.080$ | $28.727\pm 0.085$ | 0.000 | $17.6678\pm 0.0030$ |  |
4522 A | $4.4347\pm 0.0820$ | $-44.513\pm 0.122$ | $-32.865\pm 0.058$ | 0.039 | $16.8183\pm 0.0029$ | $0.3520^{+0.0934}_{-0.0951}$ |
4522 B | $4.6178\pm 0.1908$ | $-43.880\pm 0.270$ | $-32.646\pm 0.135$ | 0.000 | $18.4140\pm 0.0032$ |  |
4546 B | $3.0908\pm 0.0189$ | $-12.745\pm 0.019$ | $-4.971\pm 0.016$ | 0.081 | $10.3908\pm 0.0028$ |  |
4546 A | $3.0928\pm 0.0179$ | $-12.969\pm 0.019$ | $-4.561\pm 0.017$ | 0.087 | $10.2763\pm 0.0028$ | $0.5792^{+0.2598}_{-0.2598}$ | SHC

Table 3: continued

CTOI | $\pi$ | $\mu_{\alpha}\,cos(\delta)$ | $\mu_{\delta}$ | $epsi$ | $G$ | $A_{G}$ |
---|---|---|---|---|---|---|---
| [mas] | [mas/yr] | [mas/yr] | [mas] | [mag] | [mag] |
13073396 A | $13.6999\pm 0.0201$ | $233.697\pm 0.019$ | $-43.183\pm 0.021$ | 0.000 | $14.2910\pm 0.0028$ | $0.3730^{+0.0630}_{-0.0795}$ |
13073396 B | $13.7098\pm 0.0707$ | $233.767\pm 0.068$ | $-43.338\pm 0.076$ | 0.208 | $16.9415\pm 0.0029$ |  |
37652870 A | $8.5465\pm 0.0199$ | $37.417\pm 0.028$ | $-95.894\pm 0.015$ | 0.111 | $11.8993\pm 0.0028$ | $0.2420^{+0.1480}_{-0.2180}$ |
37652870 B | $8.5967\pm 0.0641$ | $37.070\pm 0.093$ | $-95.310\pm 0.047$ | 0.000 | $16.5463\pm 0.0029$ |  |
94984950 A | $6.4511\pm 0.0353$ | $-19.187\pm 0.045$ | $-17.146\pm 0.036$ | 0.239 |  $8.5150\pm 0.0028$ | $0.4095^{+0.2060}_{-0.2225}$ |
94984950 B | $6.2177\pm 0.3024$ | $-19.341\pm 0.362$ | $-16.500\pm 0.294$ | 1.448 | $18.8199\pm 0.0046$ |  |
145601161 A | $7.6210\pm 0.0164$ | $-33.385\pm 0.019$ | $19.478\pm 0.019$ | 0.117 |  $7.8660\pm 0.0028$ |  |
145601161 B | $7.5985\pm 0.0239$ | $-34.139\pm 0.027$ | $19.929\pm 0.027$ | 0.000 | $15.4224\pm 0.0028$ | $0.5163^{+0.5638}_{-0.3434}$ |
219018744 A | $2.7303\pm 0.0118$ | $-19.052\pm 0.014$ |  $2.823\pm 0.014$ | 0.118 | $11.2881\pm 0.0028$ |  |
219018744 B | $2.7549\pm 0.0165$ | $-18.928\pm 0.019$ |  $2.574\pm 0.019$ | 0.057 | $14.6660\pm 0.0028$ | $1.2060^{+0.3447}_{-0.3380}$ |
228463329 A | $18.3964\pm 0.0171$ | $-39.288\pm 0.022$ | $-139.784\pm 0.015$ | 0.088 |  $9.0851\pm 0.0028$ |  |
228463329 B | $18.0229\pm 0.0405$ | $-34.876\pm 0.049$ | $-142.324\pm 0.038$ | 0.235 | $14.8987\pm 0.0028$ | $0.2842^{+0.3738}_{-0.0872}$ |
248960573 A | $4.8017\pm 0.0329$ | $20.737\pm 0.036$ | $-10.531\pm 0.015$ | 0.219 | $11.9581\pm 0.0028$ |  |
248960573 B | $4.5996\pm 0.0466$ | $18.458\pm 0.061$ | $-11.062\pm 0.018$ | 0.234 | $12.7345\pm 0.0029$ |  |
323717669 A | $2.1779\pm 0.0446$ |  $6.139\pm 0.048$ | $-1.741\pm 0.041$ | 0.349 | $15.6208\pm 0.0031$ |  |
323717669 B | $2.0469\pm 0.0915$ |  $5.543\pm 0.119$ | $-2.040\pm 0.076$ | 0.330 | $17.4829\pm 0.0033$ | $0.0000^{+0.0405}_{-0.0000}$ | SHC
333785427 A | $2.5728\pm 0.0159$ | $18.637\pm 0.022$ | $16.588\pm 0.017$ | 0.098 | $10.5174\pm 0.0028$ |  |
333785427 B | $2.4686\pm 0.0533$ | $19.464\pm 0.096$ | $17.080\pm 0.060$ | 0.372 | $14.3363\pm 0.0035$ | $0.0000^{+0.4962}_{-0.0000}$ | SHC
345327044 A | $4.8734\pm 0.0124$ | $-5.968\pm 0.011$ | $-1.929\pm 0.012$ | 0.070 |  $9.7515\pm 0.0028$ |  |
345327044 B | $4.8611\pm 0.0534$ | $-5.899\pm 0.051$ | $-2.238\pm 0.047$ | 0.000 | $16.8535\pm 0.0028$ | $0.1682^{+0.0769}_{-0.1473}$ |

Table 4: This table lists for each detected companion (sorted by its
identifier) the angular separation $\rho$ and position angle $PA$ to the
associated (C)TOI, the difference between its parallax and that of the (C)TOI
$\Delta\pi$ with its significance (in brackets calculated also by taking into
account the Gaia astrometric excess noise), the differential proper motion
$\mu_{\rm rel}$ of the companion relative to the (C)TOI with its significance,
as well as its $cpm$-$index$. The last column indicates ($\star$) if the
detected companion is not listed in the WDS as companion(-candidate) of the
(C)TOI.

TOI | $\rho$ | $PA$ | $\Delta\pi$ |  $sig$- | $\mu_{\rm rel}$ |  $sig$- |  $cpm$- | not in
---|---|---|---|---|---|---|---|---
| [arcsec] | [∘] | [mas] | $\Delta\pi$ | [mas/yr] | $\mu_{\rm rel}$ | $index$ | WDS
2689 B | $7.17645\pm 0.00003$ | $198.47578\pm 0.00023$ | $0.05\pm 0.04$ | 1.1 (1.1) | $0.13\pm 0.05$ | 2.9 | 438 | $\star$
2690 A | $25.66048\pm 0.00002$ | $223.43721\pm 0.00004$ | $0.05\pm 0.03$ | 1.8 (0.3) | $0.44\pm 0.03$ | 16.9 | 61 |
2690 C | $1.88688\pm 0.00002$ | $101.16665\pm 0.00084$ | $0.17\pm 0.04$ | 4.8 (0.8) | $0.86\pm 0.04$ | 22.0 | 31 |
2690 D | $24.62012\pm 0.00004$ | $228.07745\pm 0.00009$ | $0.05\pm 0.05$ | 0.9 (0.1) | $2.41\pm 0.06$ | 43.4 | 12 | $\star$
2713 B | $3.24708\pm 0.00004$ | $350.21217\pm 0.00065$ | $0.01\pm 0.05$ | 0.1 (0.1) | $0.69\pm 0.05$ | 15.3 | 62 | $\star$
2774 B | $8.56139\pm 0.00008$ | $169.14922\pm 0.00054$ | $0.02\pm 0.12$ | 0.2 (0.0) | $1.07\pm 0.10$ | 10.9 | 15 | $\star$
2803 B | $19.53826\pm 0.00001$ |  $36.35171\pm 0.00003$ | $0.00\pm 0.02$ | 0.0 (0.0) | $0.08\pm 0.01$ | 5.4 | 304 |
2816 A | $9.53407\pm 0.00001$ | $170.70583\pm 0.00008$ | $0.04\pm 0.02$ | 2.2 (0.6) | $0.49\pm 0.02$ | 27.8 | 77 | $\star$
2892 B | $2.95539\pm 0.00004$ | $357.17196\pm 0.00081$ | $0.10\pm 0.04$ | 2.2 (0.2) | $0.94\pm 0.06$ | 15.5 | 22 | $\star$
2909 B | $2.70811\pm 0.00008$ | $264.98418\pm 0.00211$ | $0.48\pm 0.12$ | 4.0 (0.4) | $0.40\pm 0.13$ | 3.1 | 54 | $\star$
2911 B | $2.26739\pm 0.00004$ |  $66.80964\pm 0.00118$ | $0.05\pm 0.05$ | 1.1 (0.1) | $0.23\pm 0.05$ | 4.4 | 451 | $\star$
2956 B | $19.44621\pm 0.00009$ |  $34.36312\pm 0.00026$ | $0.11\pm 0.10$ | 1.1 (0.6) | $0.30\pm 0.12$ | 2.5 | 104 | $\star$
3039 B | $21.63875\pm 0.00027$ | $142.41055\pm 0.00068$ | $0.19\pm 0.29$ | 0.7 (0.2) | $3.72\pm 0.35$ | 10.8 | 13 | $\star$
3040 B | $3.45514\pm 0.00001$ | $301.42787\pm 0.00020$ | $0.01\pm 0.01$ | 1.0 (0.2) | $0.17\pm 0.02$ | 10.9 | 397 |
3073 B | $0.82393\pm 0.00006$ | $266.49870\pm 0.00874$ | $0.23\pm 0.12$ | 2.0 (0.3) | $6.98\pm 0.11$ | 65.3 | 27 | $\star$
3097 B | $1.38787\pm 0.00003$ | $146.25381\pm 0.00104$ | $0.01\pm 0.04$ | 0.2 (0.1) | $0.39\pm 0.04$ | 10.1 | 158 | $\star$
3106 B | $7.33242\pm 0.00012$ |  $50.91045\pm 0.00087$ | $0.30\pm 0.15$ | 2.0 (0.7) | $7.69\pm 0.17$ | 45.7 | 10 | $\star$
3106 C | $2.28695\pm 0.00024$ |  $12.33189\pm 0.00517$ | $0.11\pm 0.28$ | 0.4 (0.2) | $0.64\pm 0.35$ | 1.8 | 111 | $\star$
3106 D | $8.89263\pm 0.00026$ |  $49.51842\pm 0.00163$ | $0.12\pm 0.33$ | 0.4 (0.2) | $7.91\pm 0.36$ | 22.1 | 10 | $\star$
3155 B | $33.36339\pm 0.00004$ | $122.33834\pm 0.00007$ | $0.02\pm 0.06$ | 0.2 (0.2) | $0.13\pm 0.05$ | 2.6 | 449 | $\star$
3159 B | $4.18948\pm 0.00004$ | $351.10910\pm 0.00062$ | $0.05\pm 0.06$ | 0.8 (0.2) | $0.07\pm 0.05$ | 1.2 | 486 | $\star$
3179 B | $1.02289\pm 0.00005$ | $358.32287\pm 0.00344$ | $0.02\pm 0.07$ | 0.2 (0.1) | $1.27\pm 0.11$ | 11.9 | 33 | $\star$
3202 B | $6.55316\pm 0.00011$ | $223.68858\pm 0.00099$ | $0.14\pm 0.15$ | 1.0 (0.6) | $0.20\pm 0.16$ | 1.2 | 211 | $\star$
3205 B | $2.02292\pm 0.00007$ | $179.66562\pm 0.00238$ | $0.05\pm 0.09$ | 0.6 (0.1) | $1.40\pm 0.10$ | 14.1 | 194 | $\star$
3250 B | $2.14908\pm 0.00011$ | $327.62262\pm 0.00280$ | $0.11\pm 0.15$ | 0.7 (0.2) | $0.58\pm 0.15$ | 4.0 | 98 | $\star$
3252 B | $14.15443\pm 0.00002$ | $204.11227\pm 0.00009$ | $0.02\pm 0.03$ | 0.7 (0.2) | $0.09\pm 0.03$ | 3.2 | 1473 |
3266 B | $1.10865\pm 0.00004$ | $331.04209\pm 0.00204$ | $0.03\pm 0.03$ | 1.0 (0.1) | $0.47\pm 0.05$ | 9.6 | 60 | $\star$
3277 B | $2.27516\pm 0.00005$ | $337.83142\pm 0.00114$ | $0.08\pm 0.07$ | 1.2 (0.2) | $0.24\pm 0.05$ | 4.7 | 1031 | $\star$
3284 B | $3.99765\pm 0.00021$ | $309.41286\pm 0.00303$ | $0.17\pm 0.26$ | 0.7 (0.2) | $0.13\pm 0.26$ | 0.5 | 64 | $\star$
3288 B | $2.16795\pm 0.00008$ |  $24.08708\pm 0.00228$ | $0.42\pm 0.12$ | 3.4 (0.9) | $0.89\pm 0.08$ | 11.7 | 49 | $\star$
3294 B | $1.89610\pm 0.00002$ | $133.59492\pm 0.00055$ | $0.11\pm 0.03$ | 3.7 (0.6) | $0.99\pm 0.02$ | 48.2 | 21 | $\star$
3314 B | $2.27769\pm 0.00009$ | $199.87840\pm 0.00238$ | $0.22\pm 0.10$ | 2.2 (0.6) | $1.08\pm 0.11$ | 10.2 | 14 | $\star$
3342 A | $22.32103\pm 0.00002$ |  $91.13391\pm 0.00005$ | $0.07\pm 0.03$ | 2.3 (0.4) | $0.08\pm 0.02$ | 3.4 | 687 | $\star$
3344 B | $2.19552\pm 0.00004$ | $331.34953\pm 0.00105$ | $0.04\pm 0.06$ | 0.8 (0.3) | $0.95\pm 0.05$ | 17.6 | 21 | $\star$
3353 B | $102.62278\pm 0.00003$ | $100.37374\pm 0.00002$ | $0.01\pm 0.03$ | 0.2 (0.0) | $2.67\pm 0.04$ | 63.4 | 30 | $\star$
3355 B | $2.33226\pm 0.00010$ | $318.04192\pm 0.00245$ | $0.32\pm 0.10$ | 3.2 (0.7) | $0.33\pm 0.13$ | 2.5 | 238 | $\star$
3386 B | $4.46341\pm 0.00027$ | $201.05920\pm 0.00311$ | $0.47\pm 0.31$ | 1.5 (0.7) | $0.37\pm 0.29$ | 1.3 | 21 | $\star$
3398 B | $6.02272\pm 0.00017$ | $136.22144\pm 0.00164$ | $0.19\pm 0.21$ | 0.9 (0.3) | $1.18\pm 0.16$ | 7.5 | 122 | $\star$
3444 B | $3.17404\pm 0.00031$ | $181.89753\pm 0.00812$ | $0.07\pm 0.54$ | 0.1 (0.1) | $1.88\pm 0.56$ | 3.3 | 12 | $\star$
3450 B | $0.88187\pm 0.00006$ | $248.86655\pm 0.00454$ | $0.50\pm 0.08$ | 6.0 (0.8) | $1.28\pm 0.10$ | 12.8 | 37 | $\star$
3490 A | $7.60632\pm 0.00001$ | $321.25483\pm 0.00010$ | $0.01\pm 0.01$ | 0.5 (0.1) | $1.01\pm 0.02$ | 58.4 | 46 | $\star$
3491 B | $15.15459\pm 0.00013$ |  $71.90827\pm 0.00035$ | $0.14\pm 0.15$ | 0.9 (0.1) | $0.84\pm 0.19$ | 4.4 | 39 | $\star$
3492 B | $46.69394\pm 0.00131$ | $297.58032\pm 0.00165$ | $0.88\pm 1.22$ | 0.7 (0.3) | $0.19\pm 1.56$ | 0.1 | 93 | $\star$

Table 4: continued

TOI | $\rho$ | $PA$ | $\Delta\pi$ |  $sig$- | $\mu_{\rm rel}$ |  $sig$- |  $cpm$- | not in
---|---|---|---|---|---|---|---|---
| [arcsec] | [∘] | [mas] | $\Delta\pi$ | [mas/yr] | $\mu_{\rm rel}$ | $index$ | WDS
3500 B | $3.73911\pm 0.00002$ |  $34.58936\pm 0.00043$ | $0.02\pm 0.04$ | 0.4 (0.1) | $2.14\pm 0.04$ | 54.5 | 65 | $\star$
3503 A | $5.71345\pm 0.00002$ | $149.90553\pm 0.00026$ | $0.04\pm 0.03$ | 1.3 (0.1) | $0.92\pm 0.04$ | 26.1 | 32 |
3504 A | $17.69730\pm 0.00001$ | $260.57265\pm 0.00004$ | $0.03\pm 0.02$ | 1.8 (0.3) | $0.11\pm 0.01$ | 7.3 | 212 |
3514 B | $1.75837\pm 0.00004$ | $106.70558\pm 0.00180$ | $0.01\pm 0.06$ | 0.2 (0.0) | $0.65\pm 0.07$ | 10.1 | 45 | $\star$
3522 B | $3.74943\pm 0.00001$ | $220.37650\pm 0.00021$ | $0.02\pm 0.02$ | 0.9 (0.9) | $0.19\pm 0.02$ | 10.4 | 83 | $\star$
3531 B | $5.35685\pm 0.00035$ | $280.59376\pm 0.00490$ | $0.28\pm 0.42$ | 0.7 (0.2) | $0.73\pm 0.60$ | 1.2 | 64 | $\star$
3533 A | $2.53039\pm 0.00056$ | $283.10339\pm 0.01415$ | $1.82\pm 0.82$ | 2.2 (0.2) | $4.27\pm 0.77$ | 5.5 | 6.9 | $\star$
3560 B | $32.09228\pm 0.00009$ | $215.70110\pm 0.00016$ | $0.21\pm 0.10$ | 2.0 (0.2) | $1.28\pm 0.14$ | 9.3 | 10 | $\star$
3584 B | $1.09294\pm 0.00003$ | $349.04279\pm 0.00229$ | $0.02\pm 0.04$ | 0.5 (0.0) | $0.67\pm 0.04$ | 15.8 | 58 | $\star$
3584 C | $10.42956\pm 0.00005$ |  $11.69081\pm 0.00029$ | $0.01\pm 0.06$ | 0.2 (0.0) | $0.51\pm 0.07$ | 7.4 | 75 | $\star$
3586 B | $26.01437\pm 0.00010$ |  $50.04982\pm 0.00022$ | $0.13\pm 0.11$ | 1.2 (0.3) | $0.76\pm 0.12$ | 6.3 | 45 | $\star$
3607 B | $0.86206\pm 0.00006$ |  $36.18836\pm 0.00398$ | $0.04\pm 0.05$ | 0.9 (0.1) | $1.04\pm 0.09$ | 12.2 | 27 | $\star$
3628 B | $22.34937\pm 0.00001$ | $214.12449\pm 0.00004$ | $0.01\pm 0.02$ | 0.5 (0.1) | $0.35\pm 0.02$ | 21.6 | 227 |
3628 C | $21.69589\pm 0.00033$ | $211.11492\pm 0.00057$ | $0.01\pm 0.11$ | 0.1 (0.0) | $2.09\pm 0.33$ | 6.4 | 38 | $\star$
3634 B | $0.36604\pm 0.00024$ | $167.70988\pm 0.08003$ | $0.39\pm 0.42$ | 0.9 (0.2) | $2.13\pm 0.45$ | 4.7 | 8.0 | $\star$
3636 B | $2.97490\pm 0.00087$ | $294.86060\pm 0.01023$ | $3.50\pm 0.98$ | 3.6 (2.0) | $2.18\pm 0.80$ | 2.7 | 17 | $\star$
3642 B | $2.03556\pm 0.00007$ | $170.81970\pm 0.00243$ | $0.26\pm 0.10$ | 2.6 (0.8) | $0.79\pm 0.10$ | 8.0 | 37 | $\star$
3682 B | $21.81466\pm 0.00004$ | $334.66086\pm 0.00013$ | $0.26\pm 0.06$ | 4.6 (2.9) | $5.32\pm 0.05$ | 111.6 | 15 | $\star$
3688 B | $4.96403\pm 0.00016$ | $336.69639\pm 0.00144$ | $0.00\pm 0.18$ | 0.0 (0.0) | $0.28\pm 0.24$ | 1.2 | 155 | $\star$
3712 B | $25.97798\pm 0.00009$ | $325.50149\pm 0.00020$ | $0.19\pm 0.12$ | 1.6 (1.3) | $0.21\pm 0.08$ | 2.5 | 199 | $\star$
3714 B | $2.66971\pm 0.00019$ | $106.41590\pm 0.00263$ | $0.01\pm 0.23$ | 0.0 (0.0) | $1.02\pm 0.25$ | 4.1 | 143 | $\star$
3724 B | $1.72747\pm 0.00024$ | $247.92145\pm 0.00673$ | $0.66\pm 0.33$ | 2.0 (0.7) | $0.47\pm 0.36$ | 1.3 | 83 | $\star$
3741 B | $1.69562\pm 0.00016$ | $263.30954\pm 0.00438$ | $0.75\pm 0.21$ | 3.6 (0.4) | $0.59\pm 0.20$ | 2.9 | 3.7 | $\star$
3742 A | $3.70115\pm 0.00002$ | $358.27300\pm 0.00029$ | $0.01\pm 0.02$ | 0.6 (0.2) | $0.93\pm 0.02$ | 38.8 | 108 | $\star$
3745 B | $1.84484\pm 0.00003$ |  $79.16503\pm 0.00068$ | $0.03\pm 0.04$ | 0.8 (0.2) | $0.93\pm 0.04$ | 25.9 | 44 | $\star$
3758 B | $1.24652\pm 0.00008$ | $204.94901\pm 0.00362$ | $0.07\pm 0.10$ | 0.7 (0.2) | $1.21\pm 0.12$ | 10.0 | 12 | $\star$
3761 A | $4.99206\pm 0.00001$ |  $12.41282\pm 0.00010$ | $0.01\pm 0.02$ | 0.7 (0.3) | $1.09\pm 0.01$ | 96.5 | 57 | $\star$
3781 B | $12.68772\pm 0.00003$ | $151.58995\pm 0.00013$ | $0.01\pm 0.04$ | 0.2 (0.1) | $1.33\pm 0.04$ | 36.7 | 38 | $\star$
3791 B | $9.68258\pm 0.00001$ | $187.37463\pm 0.00007$ | $0.03\pm 0.01$ | 2.0 (0.3) | $0.05\pm 0.02$ | 2.8 | 621 |
3795 B | $8.57354\pm 0.00005$ | $201.24130\pm 0.00036$ | $0.06\pm 0.07$ | 0.9 (0.3) | $0.23\pm 0.06$ | 3.9 | 12 | $\star$
3797 B | $8.88802\pm 0.00003$ |  $35.96399\pm 0.00016$ | $0.02\pm 0.03$ | 0.5 (0.2) | $0.36\pm 0.03$ | 11.5 | 59 | $\star$
3801 B | $2.93556\pm 0.00015$ | $359.74432\pm 0.00342$ | $0.19\pm 0.23$ | 0.8 (0.3) | $0.18\pm 0.19$ | 0.9 | 172 | $\star$
3823 B | $3.32667\pm 0.00017$ | $264.78039\pm 0.00325$ | $0.43\pm 0.24$ | 1.8 (0.4) | $0.75\pm 0.21$ | 3.6 | 40 | $\star$
3828 B | $1.44861\pm 0.00001$ | $328.16529\pm 0.00055$ | $0.05\pm 0.02$ | 2.5 (0.3) | $0.81\pm 0.02$ | 41.4 | 94 | $\star$
3829 B | $1.47567\pm 0.00007$ |  $56.87083\pm 0.00261$ | $0.29\pm 0.08$ | 3.6 (1.1) | $3.00\pm 0.11$ | 26.3 | 15 | $\star$
3867 B | $2.73594\pm 0.00015$ | $190.79063\pm 0.00362$ | $0.12\pm 0.23$ | 0.5 (0.1) | $0.26\pm 0.23$ | 1.1 | 242 | $\star$
3872 B | $2.37493\pm 0.00005$ | $245.35337\pm 0.00108$ | $0.02\pm 0.06$ | 0.4 (0.1) | $0.55\pm 0.05$ | 10.6 | 110 | $\star$
3875 B | $18.14488\pm 0.00004$ |  $22.79862\pm 0.00012$ | $0.15\pm 0.04$ | 3.7 (0.4) | $0.22\pm 0.05$ | 4.7 | 220 | $\star$
3883 B | $5.24150\pm 0.00004$ |  $81.33593\pm 0.00062$ | $0.08\pm 0.09$ | 1.0 (0.2) | $0.24\pm 0.05$ | 5.0 | 97 | $\star$
3889 B | $2.27171\pm 0.00002$ | $265.57761\pm 0.00062$ | $0.03\pm 0.03$ | 1.0 (0.2) | $1.92\pm 0.03$ | 60.2 | 48 | $\star$
3896 B | $17.87801\pm 0.00003$ | $122.79499\pm 0.00008$ | $0.04\pm 0.03$ | 1.4 (0.4) | $0.08\pm 0.03$ | 2.3 | 2762 |
3915 B | $1.70971\pm 0.00016$ | $268.19507\pm 0.00396$ | $0.01\pm 0.19$ | 0.1 (0.0) | $1.34\pm 0.15$ | 8.7 | 77 | $\star$
3920 B | $1.68308\pm 0.00002$ | $190.40474\pm 0.00091$ | $0.01\pm 0.03$ | 0.3 (0.1) | $0.16\pm 0.03$ | 4.9 | 150 | $\star$
3922 A | $2.08039\pm 0.00002$ | $225.86255\pm 0.00045$ | $0.00\pm 0.02$ | 0.2 (0.0) | $0.80\pm 0.02$ | 48.4 | 134 | $\star$
3956 A | $4.08617\pm 0.00002$ | $265.86837\pm 0.00036$ | $0.02\pm 0.03$ | 0.8 (0.1) | $1.18\pm 0.03$ | 36.2 | 16 | $\star$
3966 B | $2.81173\pm 0.00019$ |  $56.91994\pm 0.00398$ | $0.53\pm 0.27$ | 2.0 (0.2) | $1.00\pm 0.25$ | 4.0 | 38 | $\star$
3977 B | $2.95021\pm 0.00001$ |  $46.82758\pm 0.00025$ | $0.01\pm 0.01$ | 0.9 (0.2) | $0.57\pm 0.02$ | 28.4 | 217 | $\star$

Table 4: continued

TOI | $\rho$ | $PA$ | $\Delta\pi$ |  $sig$- | $\mu_{\rm rel}$ |  $sig$- |  $cpm$- | not in
---|---|---|---|---|---|---|---|---
| [arcsec] | [∘] | [mas] | $\Delta\pi$ | [mas/yr] | $\mu_{\rm rel}$ | $index$ | WDS
3984 B | $3.27064\pm 0.00015$ | $343.07874\pm 0.00231$ | $0.13\pm 0.20$ | 0.6 (0.6) | $2.22\pm 0.19$ | 11.4 | 59 | $\star$
3998 B | $2.16139\pm 0.00003$ |  $54.20794\pm 0.00096$ | $0.05\pm 0.05$ | 0.9 (0.2) | $0.48\pm 0.05$ | 9.7 | 167 | $\star$
4001 B | $10.33196\pm 0.00001$ | $307.08633\pm 0.00008$ | $0.00\pm 0.02$ | 0.1 (0.1) | $0.42\pm 0.02$ | 22.6 | 186 | $\star$
4021 B | $11.36437\pm 0.00002$ | $251.72711\pm 0.00009$ | $0.01\pm 0.03$ | 0.3 (0.1) | $1.00\pm 0.02$ | 44.5 | 27 | $\star$
4040 B | $3.35613\pm 0.00120$ |  $8.87701\pm 0.01400$ | $1.79\pm 0.96$ | 1.9 (0.6) | $5.12\pm 2.14$ | 2.4 | 6.5 | $\star$
4059 B | $3.53855\pm 0.00010$ | $218.08460\pm 0.00156$ | $0.22\pm 0.10$ | 2.2 (0.4) | $0.79\pm 0.14$ | 5.7 | 65 | $\star$
4070 A | $3.74492\pm 0.00002$ |  $27.88078\pm 0.00032$ | $0.20\pm 0.02$ | 8.4 (0.8) | $0.72\pm 0.03$ | 28.6 | 57 | $\star$
4077 B | $15.58884\pm 0.00008$ |  $37.90108\pm 0.00028$ | $0.02\pm 0.09$ | 0.2 (0.2) | $0.39\pm 0.11$ | 3.6 | 78 | $\star$
4079 A | $11.46628\pm 0.00001$ | $225.03099\pm 0.00005$ | $0.02\pm 0.02$ | 1.2 (0.3) | $0.29\pm 0.01$ | 19.8 | 124 | $\star$
4081 B | $2.17240\pm 0.00002$ | $257.98470\pm 0.00063$ | $0.06\pm 0.03$ | 1.9 (0.3) | $0.77\pm 0.03$ | 23.3 | 48 | $\star$
4089 B | $1.15891\pm 0.00002$ |  $58.38509\pm 0.00123$ | $0.06\pm 0.04$ | 1.8 (0.3) | $0.63\pm 0.04$ | 15.8 | 96 | $\star$
4107 B | $12.35119\pm 0.00004$ | $117.98406\pm 0.00016$ | $0.05\pm 0.03$ | 1.5 (0.2) | $0.27\pm 0.04$ | 6.3 | 112 | $\star$
4113 B | $3.55473\pm 0.00008$ |  $74.02587\pm 0.00142$ | $0.27\pm 0.08$ | 3.2 (0.8) | $0.57\pm 0.11$ | 5.1 | 237 | $\star$
4123 B | $2.56674\pm 0.00012$ | $359.63176\pm 0.00228$ | $0.18\pm 0.15$ | 1.2 (0.2) | $1.12\pm 0.14$ | 8.0 | 86 | $\star$
4128 B | $23.74700\pm 0.00007$ | $328.63903\pm 0.00018$ | $0.02\pm 0.09$ | 0.2 (0.0) | $0.63\pm 0.12$ | 5.3 | 102 |
4145 B | $1.74266\pm 0.00040$ |  $41.46992\pm 0.01178$ | $0.80\pm 0.16$ | 4.9 (1.2) | $3.30\pm 0.59$ | 5.6 | 12 | $\star$
4168 B | $8.56570\pm 0.00002$ | $293.72152\pm 0.00013$ | $0.07\pm 0.02$ | 3.0 (0.6) | $0.38\pm 0.03$ | 12.5 | 143 | $\star$
4175 B | $1.61034\pm 0.00004$ | $259.76981\pm 0.00139$ | $0.23\pm 0.05$ | 4.2 (0.9) | $10.31\pm 0.06$ | 186.2 | 38 |
4175 C | $166.81119\pm 0.00003$ | $178.24945\pm 0.00001$ | $0.07\pm 0.04$ | 1.5 (0.3) | $4.50\pm 0.05$ | 92.1 | 87 |
4176 B | $24.27219\pm 0.00002$ | $335.40461\pm 0.00006$ | $0.00\pm 0.03$ | 0.1 (0.0) | $0.21\pm 0.03$ | 7.0 | 111 | $\star$
4179 A | $38.08353\pm 0.00019$ | $165.02820\pm 0.00037$ | $0.56\pm 0.31$ | 1.8 (0.2) | $6.14\pm 0.25$ | 24.8 | 20 |
4182 B | $17.45414\pm 0.00004$ | $330.08316\pm 0.00013$ | $0.00\pm 0.04$ | 0.0 (0.0) | $1.00\pm 0.05$ | 18.8 | 281 | $\star$
4192 B | $2.73019\pm 0.00001$ | $288.26841\pm 0.00030$ | $0.04\pm 0.02$ | 1.9 (0.5) | $0.12\pm 0.02$ | 8.2 | 440 | $\star$
4212 B | $26.92283\pm 0.00119$ | $184.80178\pm 0.00154$ | $4.27\pm 1.49$ | 2.9 (0.4) | $1.65\pm 1.83$ | 0.9 | 6.1 | $\star$
4226 B | $5.62051\pm 0.00038$ |  $15.78624\pm 0.00280$ | $0.58\pm 0.55$ | 1.1 (0.2) | $0.98\pm 0.47$ | 2.1 | 5.1 | $\star$
4245 B | $1.65324\pm 0.00011$ | $157.97771\pm 0.00392$ | $0.12\pm 0.12$ | 1.0 (0.1) | $1.56\pm 0.16$ | 10.0 | 42 | $\star$
4293 B | $2.49352\pm 0.00008$ | $332.65097\pm 0.00234$ | $0.19\pm 0.16$ | 1.2 (0.6) | $0.49\pm 0.15$ | 3.3 | 120 | $\star$
4301 B | $34.80516\pm 0.00022$ | $104.73358\pm 0.00052$ | $0.25\pm 0.28$ | 0.9 (0.9) | $0.47\pm 0.30$ | 1.5 | 288 | $\star$
4303 B | $9.11370\pm 0.00002$ | $158.50453\pm 0.00013$ | $0.06\pm 0.02$ | 2.6 (0.4) | $0.49\pm 0.03$ | 17.5 | 188 | $\star$
4325 B | $25.29992\pm 0.00003$ | $356.26082\pm 0.00008$ | $0.02\pm 0.04$ | 0.4 (0.1) | $0.80\pm 0.04$ | 19.5 | 462 |
4330 B | $2.18530\pm 0.00010$ |  $3.90890\pm 0.00363$ | $0.11\pm 0.15$ | 0.7 (0.1) | $0.46\pm 0.15$ | 3.1 | 185 |
4337 A | $5.10545\pm 0.00002$ | $209.01323\pm 0.00019$ | $0.03\pm 0.02$ | 1.7 (0.3) | $0.57\pm 0.02$ | 26.2 | 105 |
4339 A | $3.62569\pm 0.00003$ | $162.07409\pm 0.00053$ | $0.03\pm 0.04$ | 0.7 (0.4) | $1.07\pm 0.04$ | 26.6 | 154 | $\star$
4344 B | $2.10247\pm 0.00007$ | $248.43131\pm 0.00236$ | $0.09\pm 0.07$ | 1.2 (0.1) | $1.82\pm 0.12$ | 15.8 | 25 | $\star$
4349 B | $2.68110\pm 0.00008$ |  $12.35082\pm 0.00193$ | $0.04\pm 0.11$ | 0.3 (0.0) | $3.58\pm 0.10$ | 37.5 | 167 | $\star$
4350 B | $3.80322\pm 0.00007$ | $359.59813\pm 0.00138$ | $0.15\pm 0.08$ | 1.8 (0.3) | $0.88\pm 0.13$ | 6.6 | 156 | $\star$
4359 B | $15.49053\pm 0.00003$ | $129.51739\pm 0.00012$ | $0.08\pm 0.04$ | 2.1 (1.1) | $0.75\pm 0.04$ | 18.9 | 87 | $\star$
4366 B | $19.35358\pm 0.00002$ | $325.19177\pm 0.00007$ | $0.00\pm 0.03$ | 0.1 (0.0) | $0.58\pm 0.03$ | 21.1 | 33 | $\star$
4369 B | $6.11232\pm 0.00007$ | $354.48099\pm 0.00067$ | $0.45\pm 0.07$ | 6.3 (0.5) | $1.29\pm 0.10$ | 12.7 | 55 |
4370 B | $30.52375\pm 0.00007$ |  $75.16433\pm 0.00010$ | $0.04\pm 0.08$ | 0.6 (0.2) | $1.08\pm 0.09$ | 12.3 | 38 | $\star$
4372 B | $3.48683\pm 0.00025$ | $249.86993\pm 0.00413$ | $1.14\pm 0.30$ | 3.8 (0.8) | $2.76\pm 0.36$ | 7.6 | 25 | $\star$
4390 B | $1.11151\pm 0.00005$ |  $53.91390\pm 0.00252$ | $0.01\pm 0.05$ | 0.2 (0.0) | $1.95\pm 0.06$ | 34.0 | 17 |
4414 A | $0.89987\pm 0.00014$ | $314.71208\pm 0.00859$ | $0.16\pm 0.06$ | 2.6 (0.6) | $1.29\pm 0.10$ | 12.7 | 20 |
4420 B | $4.61200\pm 0.00002$ |  $14.30015\pm 0.00024$ | $0.05\pm 0.03$ | 1.6 (0.2) | $0.88\pm 0.03$ | 34.0 | 34 |
4425 B | $5.00122\pm 0.00004$ | $205.10110\pm 0.00050$ | $0.02\pm 0.05$ | 0.4 (0.1) | $0.21\pm 0.05$ | 4.0 | 184 | $\star$
4463 B | $11.36997\pm 0.00004$ | $107.62112\pm 0.00025$ | $0.01\pm 0.07$ | 0.2 (0.1) | $0.37\pm 0.07$ | 5.0 | 275 | $\star$
4499 B | $14.56409\pm 0.00007$ | $187.77535\pm 0.00023$ | $0.02\pm 0.07$ | 0.3 (0.2) | $0.48\pm 0.08$ | 5.7 | 151 | $\star$
4522 B | $7.04849\pm 0.00018$ | $270.63678\pm 0.00111$ | $0.18\pm 0.21$ | 0.9 (0.9) | $0.67\pm 0.28$ | 2.4 | 164 | $\star$
4546 A | $7.66036\pm 0.00002$ | $207.34741\pm 0.00016$ | $0.00\pm 0.03$ | 0.1 (0.0) | $0.47\pm 0.02$ | 19.3 | 59 | $\star$

Table 4: continued

CTOI | $\rho$ | $PA$ | $\Delta\pi$ |  $sig$- | $\mu_{\rm rel}$ |  $sig$- |  $cpm$- | not in
---|---|---|---|---|---|---|---|---
| [arcsec] | [∘] | [mas] | $\Delta\pi$ | [mas/yr] | $\mu_{\rm rel}$ | $index$ | WDS
13073396 B | $67.96994\pm 0.00007$ | $214.30476\pm 0.00006$ | $0.01\pm 0.07$ | 0.1 (0.0) | $0.17\pm 0.08$ | 2.2 | 2795 |
37652870 B | $46.09297\pm 0.00006$ | $290.98867\pm 0.00006$ | $0.05\pm 0.07$ | 0.7 (0.4) | $0.68\pm 0.07$ | 10.4 | 302 |
94984950 B | $14.27266\pm 0.00028$ |  $71.24118\pm 0.00078$ | $0.23\pm 0.30$ | 0.8 (0.2) | $0.66\pm 0.30$ | 2.2 | 77 | $\star$
145601161 B | $21.98785\pm 0.00002$ | $281.75747\pm 0.00007$ | $0.02\pm 0.03$ | 0.8 (0.2) | $0.88\pm 0.03$ | 26.6 | 89 | $\star$
219018744 B | $13.34805\pm 0.00002$ | $243.02983\pm 0.00008$ | $0.02\pm 0.02$ | 1.2 (0.2) | $0.28\pm 0.02$ | 11.8 | 138 | $\star$
228463329 B | $21.27769\pm 0.00004$ | $256.02820\pm 0.00010$ | $0.37\pm 0.04$ | 8.5 (1.5) | $5.09\pm 0.05$ | 100.2 | 57 | $\star$
248960573 B | $0.83697\pm 0.00002$ |  $0.35273\pm 0.00358$ | $0.20\pm 0.06$ | 3.5 (0.6) | $2.34\pm 0.07$ | 33.8 | 19 | $\star$
323717669 B | $1.19821\pm 0.00007$ | $357.12315\pm 0.00532$ | $0.13\pm 0.10$ | 1.3 (0.3) | $0.67\pm 0.12$ | 5.5 | 18 | $\star$
333785427 B | $1.41681\pm 0.00005$ |  $21.19582\pm 0.00259$ | $0.10\pm 0.06$ | 1.9 (0.3) | $0.96\pm 0.09$ | 10.6 | 53 | $\star$
345327044 B | $27.39360\pm 0.00004$ | $222.34293\pm 0.00008$ | $0.01\pm 0.05$ | 0.2 (0.1) | $0.32\pm 0.05$ | 6.5 | 40 | $\star$

Table 5: This table lists the equatorial coordinates ($\alpha$, $\delta$ for
epoch 2016.0) of all detected co-moving companions (sorted by their
identifier) together with their derived absolute G-band magnitude $M_{\rm G}$,
projected separation $sep$, mass, and effective temperature $T_{\rm eff}$. The
flags for all companions, as defined in the text, are listed in the last
column of this table.

TOI | $\alpha$ | $\delta$ | $M_{\rm G}$ | $sep$ | $mass$ | $T_{\rm eff}$ | Flags
---|---|---|---|---|---|---|---
| [∘] | [∘] | [mag] | [au] | [$M_{\odot}$] | [K] |
2689 B | 52.67980914211 | -22.00574100448 | $8.60^{+0.24}_{-0.39}$ | 2293 | $0.55^{+0.05}_{-0.01}$ | $3644^{+74}_{-30}$ |  PRI BPRP
2690 A | 52.22564042075 | -19.97980931517 | $3.06^{+0.28}_{-0.27}$ | 5675 | $1.25^{+0.15}_{-0.19}$ | $6582^{+499}_{-422}$ |  PRI BPRP
2690 C | 52.23140217705 | -19.97473504235 | $6.17^{+0.02}_{-0.23}$ | 417 | $0.72^{+0.11}_{-0.10}$ | $5091^{+587}_{-491}$ | BPRP
2690 D | 52.22544078874 | -19.97920279422 | $7.82^{+0.02}_{-0.23}$ | 5445 | $0.57^{+0.18}_{-0.16}$ | $4119^{+1011}_{-591}$ |
2713 B | 63.14997314217 | -12.31677269638 | $9.38^{+0.17}_{-0.10}$ | 803 | $0.50^{+0.01}_{-0.01}$ | $3439^{+43}_{-18}$ | BPRP
2774 B | 83.99328101402 | -7.69070839901 | $6.38^{+0.13}_{-0.13}$ | 4387 | $0.77^{+0.03}_{-0.03}$ | $4663^{+87}_{-130}$ |  PRI BPRP
2803 B | 93.11824755581 | -23.48812274817 | $4.26^{+0.03}_{-0.10}$ | 9656 | $0.98^{+0.10}_{-0.11}$ | $6127^{+268}_{-255}$ |  PRI BPRP
2816 A | 118.34827052025 | -36.80303124411 | $3.39^{+0.29}_{-0.16}$ | 4802 | $1.05^{+0.19}_{-0.11}$ | $6124^{+410}_{-432}$ |  PRI BPRP
2892 B | 116.21354153938 | -59.55033254810 | $6.97^{+0.12}_{-0.08}$ | 1134 | $0.77^{+0.02}_{-0.07}$ | $4144^{+133}_{-140}$ |  PRI BPRP SHC2
2909 B | 135.66762775837 | -37.01688685089 | $4.98^{+0.16}_{-0.15}$ | 1471 | $0.89^{+0.07}_{-0.08}$ | $5950^{+336}_{-341}$ | BPRP
2911 B | 129.08112322060 | -46.36535231381 | $8.74^{+0.48}_{-0.48}$ | 408 | $0.46^{+0.04}_{-0.01}$ | $3759^{+236}_{-217}$ | BPRP
2956 B | 154.07230985168 | -55.70815920608 | $10.22^{+0.10}_{-0.11}$ | 7006 | $0.35^{+0.01}_{-0.01}$ | $3397^{+21}_{-20}$ |  BPRP inter
3039 B | 153.13022050881 | -67.26030381008 | $10.92^{+0.12}_{-0.15}$ | 9581 | $0.26^{+0.02}_{-0.01}$ | $3261^{+28}_{-21}$ |  BPRP inter
3040 B | 151.49952902222 | -66.89749884226 | $4.02^{+0.09}_{-0.17}$ | 1587 | $1.04^{+0.10}_{-0.12}$ | $6332^{+335}_{-321}$ |  PRI BPRP
3073 B | 46.56549356037 | 70.21466583708 | $10.35^{+0.01}_{-0.06}$ | 51 | $0.31^{+0.15}_{-0.10}$ | $3393^{+328}_{-277}$ |
3097 B | 173.07501259364 | -47.49670805769 | $8.28^{+0.02}_{-0.35}$ | 576 | $0.53^{+0.20}_{-0.16}$ | $3943^{+1022}_{-504}$ | BPRP
3106 B | 198.65051016909 | -30.72143684476 | $10.03^{+0.04}_{-0.04}$ | 2951 | $0.37^{+0.01}_{-0.01}$ | $3432^{+5}_{-6}$ |  BPRP inter
3106 C | 198.64882903573 | -30.72210050023 | $10.45^{+0.04}_{-0.04}$ | 920 | $0.32^{+0.01}_{-0.01}$ | $3352^{+8}_{-8}$ | inter
3106 D | 198.65085679278 | -30.72111745904 | $11.32^{+0.04}_{-0.04}$ | 3579 | $0.22^{+0.01}_{-0.01}$ | $3197^{+5}_{-5}$ | inter
3155 B | 203.54694265012 | -59.58056427971 | $9.97^{+0.20}_{-0.26}$ | 6699 | $0.40^{+0.01}_{-0.15}$ | $3277^{+51}_{-150}$ | BPRP
3159 B | 200.46403486980 | -62.54097288469 | $7.37^{+0.41}_{-0.41}$ | 1803 | $0.60^{+0.05}_{-0.04}$ | $4403^{+400}_{-233}$ | BPRP
3179 B | 155.14254447665 | -62.65066542031 | $6.10^{+0.02}_{-0.50}$ | 457 | $0.73^{+0.21}_{-0.16}$ | $5078^{+875}_{-971}$ |
3202 B | 212.54548867172 | -51.45435224644 | $10.14^{+0.12}_{-0.12}$ | 2496 | $0.44^{+0.02}_{-0.03}$ | $3249^{+42}_{-51}$ |  BPRP SHC2
3205 B | 218.47574830405 | -24.65345918341 | $10.37^{+0.28}_{-0.50}$ | 500 | $0.31^{+0.14}_{-0.11}$ | $3381^{+338}_{-275}$ |
3250 B | 210.09591253907 | -22.34183472940 | $4.89^{+0.45}_{-0.33}$ | 908 | $0.91^{+0.10}_{-0.09}$ | $5748^{+428}_{-364}$ |  PRI BPRP
3252 B | 209.18350344891 | -35.29244923624 | $6.33^{+0.18}_{-0.35}$ | 3892 | $0.77^{+0.03}_{-0.03}$ | $4802^{+160}_{-126}$ |  PRI BPRP
3266 B | 270.94813182446 | -86.30896563367 | $5.35^{+0.03}_{-0.50}$ | 564 | $0.82^{+0.22}_{-0.18}$ | $5513^{+765}_{-1020}$ |
3277 B | 290.85656623835 | -54.33008049712 | $7.36^{+0.46}_{-0.46}$ | 621 | $0.60^{+0.05}_{-0.05}$ | $4345^{+251}_{-371}$ | BPRP
3284 B | 295.19066454851 | -49.41967226418 | $10.00^{+0.15}_{-0.19}$ | 1949 | $0.37^{+0.01}_{-0.02}$ | $3435^{+20}_{-25}$ |  BPRP inter
3288 B | 297.11065076211 | -43.01745378499 | $9.33^{+0.32}_{-0.17}$ | 436 | $0.39^{+0.01}_{-0.04}$ | $3711^{+183}_{-206}$ | BPRP
3294 B | 279.64123193685 | -62.30216351727 | $5.18^{+0.49}_{-0.43}$ | 655 | $0.84^{+0.24}_{-0.19}$ | $5595^{+757}_{-975}$ |
3314 B | 279.61040441412 | -40.80284923000 | $9.93^{+0.20}_{-0.25}$ | 1214 | $0.36^{+0.14}_{-0.15}$ | $3467^{+423}_{-316}$ |
3342 A | 266.37031019423 | -56.88307732848 | $3.17^{+0.21}_{-0.27}$ | 7548 | $1.24^{+0.14}_{-0.16}$ | $6737^{+475}_{-417}$ |  PRI BPRP
3344 B | 272.45063094575 | -31.89101009750 | $8.56^{+0.02}_{-0.32}$ | 542 | $0.50^{+0.18}_{-0.15}$ | $3833^{+832}_{-419}$ | BPRP
3353 B | 106.64429307975 | -75.82468702824 | $11.28^{+0.23}_{-0.32}$ | 8091 | $0.30^{+0.01}_{-0.01}$ | $2969^{+6}_{-6}$ |  PRI BPRP
3355 B | 79.32283332374 | -59.06790375910 | $9.79^{+0.02}_{-0.15}$ | 615 | $0.39^{+0.01}_{-0.01}$ | $3457^{+20}_{-3}$ |  BPRP inter
3386 B | 114.31707212743 | -36.27431755178 | $10.77^{+0.13}_{-0.12}$ | 2262 | $0.28^{+0.01}_{-0.02}$ | $3290^{+23}_{-25}$ |  BPRP inter
3398 B | 143.54204550775 | -7.43466051582 | $12.66^{+0.11}_{-0.17}$ | 1002 | $0.15^{+0.01}_{-0.01}$ | $3030^{+25}_{-16}$ |  BPRP inter
3444 B | 241.28746446466 | -46.56653151785 | $10.54^{+0.19}_{-0.21}$ | 1558 | $0.31^{+0.03}_{-0.02}$ | $3334^{+41}_{-37}$ |  BPRP inter
3450 B | 228.03493229226 | -53.31341707455 | $4.03^{+0.23}_{-0.23}$ | 227 | $0.98^{+0.01}_{-0.01}$ | $6098^{+124}_{-138}$ |  BPRP inter

Table 5: continued

TOI | $\alpha$ | $\delta$ | $M_{\rm G}$ | $sep$ | $mass$ | $T_{\rm eff}$ | Flags
---|---|---|---|---|---|---|---
| [∘] | [∘] | [mag] | [au] | [$M_{\odot}$] | [K] |
3490 A | 155.19220256086 | -78.83037132449 | $4.50^{+0.16}_{-0.22}$ | 2069 | $0.97^{+0.08}_{-0.08}$ | $5898^{+294}_{-255}$ |  PRI BPRP
3491 B | 245.27530424327 | -59.50924599551 | $5.76^{+0.31}_{-0.29}$ | 8216 | $0.84^{+0.03}_{-0.04}$ | $5104^{+121}_{-188}$ |  PRI BPRP
3492 B | 166.61723550293 | -53.72597472023 | $13.97^{+0.24}_{-0.26}$ | 9467 | $0.11^{+0.01}_{-0.01}$ | $2848^{+34}_{-32}$ |  BPRP inter
3500 B | 186.81755444350 | -29.83214647849 | $6.04^{+0.14}_{-0.27}$ | 720 | $0.69^{+0.01}_{-0.04}$ | $5327^{+186}_{-291}$ |  PRI BPRP
3503 A | 163.71599435291 | -58.57065780251 | $1.09^{+0.17}_{-0.08}$ | 2533 | $2.04^{+0.20}_{-0.17}$ | $9289^{+633}_{-539}$ |  PRI BPRP
3504 A | 300.72967978564 | 24.43432813004 | $3.38^{+0.38}_{-0.46}$ | 5275 | $1.15^{+0.15}_{-0.17}$ | $6255^{+434}_{-377}$ |  PRI BPRP
3514 B | 295.55733246370 | 32.61396027509 | $6.39^{+0.14}_{-0.27}$ | 735 | $0.75^{+0.05}_{-0.06}$ | $4809^{+298}_{-184}$ |
3522 B | 301.07877627007 | 34.39800696820 | $5.86^{+0.19}_{-0.19}$ | 1439 | $0.79^{+0.01}_{-0.01}$ | $5144^{+20}_{-179}$ |  PRI BPRP SHC2
3531 B | 321.37489008166 | 55.72320749049 | $11.30^{+0.28}_{-0.20}$ | 1934 | $0.23^{+0.02}_{-0.02}$ | $3199^{+30}_{-34}$ |  BPRP inter
3533 A | 308.56188357176 | 35.39520207642 | $3.88^{+0.50}_{-0.46}$ | 612 | $1.04^{+0.14}_{-0.12}$ | $6252^{+380}_{-337}$ |  PRI BPRP
3560 B | 296.05666264299 | 40.30133090433 | $6.47^{+0.10}_{-0.14}$ | 9736 | $0.75^{+0.06}_{-0.01}$ | $4684^{+97}_{-145}$ |  PRI BPRP
3584 B | 314.89532676098 | 52.39640704381 | $5.61^{+0.03}_{-0.52}$ | 483 | $0.79^{+0.22}_{-0.19}$ | $5364^{+784}_{-1068}$ |
3584 C | 314.89638340826 | 52.39894598594 | $8.45^{+0.21}_{-0.21}$ | 4610 | $0.60^{+0.01}_{-0.06}$ | $3694^{+138}_{-201}$ | BPRP
3586 B | 310.22786035232 | 50.92736379220 | $11.10^{+0.02}_{-0.18}$ | 6127 | $0.30^{+0.02}_{-0.01}$ | $3046^{+55}_{-24}$ | BPRP
3607 B | 310.70522263346 | 58.51513806732 | $6.91^{+0.04}_{-0.49}$ | 445 | $0.65^{+0.19}_{-0.17}$ | $4596^{+965}_{-842}$ |
3628 B | 12.86088057204 | 47.65766502045 | $4.10^{+0.14}_{-0.19}$ | 7458 | $0.94^{+0.13}_{-0.08}$ | $6085^{+286}_{-240}$ |  PRI BPRP
3628 C | 12.86142759059 | 47.65764466259 | $8.11^{+0.14}_{-0.19}$ | 7240 | $0.58^{+0.02}_{-0.02}$ | $3881^{+72}_{-56}$ | inter
3634 B | 12.56953489794 | 27.56870464509 | $4.03^{+0.23}_{-0.23}$ | 182 | $1.15^{+0.04}_{-0.08}$ | $6098^{+124}_{-138}$ |
3636 B | 21.06423146521 | 32.81104514730 | $10.79^{+0.19}_{-0.18}$ | 1322 | $0.28^{+0.02}_{-0.02}$ | $3286^{+35}_{-35}$ |  BPRP inter
3642 B | 45.14837045982 | 39.93455028157 | $9.81^{+0.17}_{-0.17}$ | 752 | $0.36^{+0.17}_{-0.13}$ | $3494^{+407}_{-320}$ |
3682 B | 50.27236394088 | 25.30273990370 | $6.72^{+0.22}_{-0.38}$ | 8652 | $0.65^{+0.01}_{-0.03}$ | $4741^{+170}_{-542}$ |  PRI BPRP
3688 B | 39.28139400597 | 54.85247997963 | $9.69^{+0.27}_{-0.28}$ | 1976 | $0.40^{+0.03}_{-0.02}$ | $3468^{+64}_{-28}$ |  BPRP inter
3712 B | 89.23862334799 | 36.36406003677 | $9.67^{+0.03}_{-0.03}$ | 9188 | $0.45^{+0.01}_{-0.01}$ | $3366^{+7}_{-9}$ | BPRP
3714 B | 69.55326641769 | 39.45778406803 | $13.12^{+0.15}_{-0.44}$ | 302 |  |  |  BPRP WD
3724 B | 80.42532763791 | 36.27445179215 | $7.32^{+0.14}_{-0.17}$ | 759 | $0.65^{+0.14}_{-0.10}$ | $4312^{+971}_{-420}$ | SHC2
3741 B | 81.57756446053 | 47.07372521578 | $4.70^{+0.43}_{-0.39}$ | 816 | $0.92^{+0.08}_{-0.07}$ | $5920^{+304}_{-305}$ |
3742 A | 72.79961580873 | 50.09792164393 | $6.49^{+0.42}_{-0.27}$ | 617 | $0.75^{+0.05}_{-0.02}$ | $4677^{+163}_{-97}$ |  PRI BPRP
3745 B | 65.61614638996 | 46.53610430219 | $5.20^{+0.38}_{-0.30}$ | 643 | $0.84^{+0.06}_{-0.06}$ | $5747^{+287}_{-287}$ |  PRI BPRP
3758 B | 41.32320343219 | 69.10594381977 | $9.34^{+0.49}_{-0.43}$ | 624 | $0.43^{+0.18}_{-0.17}$ | $3620^{+694}_{-359}$ |
3761 A | 48.67072130313 | 66.92212577884 | $5.33^{+0.09}_{-0.11}$ | 1087 | $0.88^{+0.04}_{-0.06}$ | $5445^{+261}_{-236}$ |  PRI BPRP
3781 B | 110.88135381827 | 50.34642062369 | $8.06^{+0.10}_{-0.53}$ | 3446 | $0.60^{+0.01}_{-0.01}$ | $3888^{+142}_{-63}$ |  PRI BPRP
3791 B | 295.38708444765 | 56.21513543548 | $3.92^{+0.17}_{-0.09}$ | 4692 | $1.07^{+0.12}_{-0.12}$ | $6262^{+378}_{-337}$ |  PRI BPRP
3795 B | 98.73110756335 | 49.67435429421 | $8.27^{+0.04}_{-0.16}$ | 3736 | $0.55^{+0.01}_{-0.01}$ | $3877^{+17}_{-17}$ |  PRI BPRP
3797 B | 104.84307868700 | 48.30487763435 | $6.58^{+0.15}_{-0.38}$ | 3563 | $0.75^{+0.05}_{-0.02}$ | $4640^{+122}_{-95}$ |  PRI BPRP
3801 B | 114.01080278850 | 47.25894442431 | $9.57^{+0.30}_{-0.14}$ | 1459 | $0.41^{+0.01}_{-0.03}$ | $3494^{+33}_{-45}$ |  BPRP inter
3823 B | 127.03203872903 | 56.43099174198 | $9.64^{+0.16}_{-0.14}$ | 1490 | $0.40^{+0.01}_{-0.01}$ | $3477^{+33}_{-21}$ |  BPRP inter
3828 B | 150.89193313396 | 67.99037362147 | $3.40^{+0.25}_{-0.25}$ | 501 | $1.29^{+0.07}_{-0.08}$ | $6457^{+176}_{-170}$ |  BPRP inter
3829 B | 137.42163520494 | 31.29264394692 | $6.07^{+0.29}_{-0.23}$ | 578 | $0.79^{+0.02}_{-0.04}$ | $4925^{+168}_{-206}$ |  BPRP inter
3867 B | 193.65507319999 | 47.06549457455 | $10.09^{+0.25}_{-0.13}$ | 1318 | $0.37^{+0.01}_{-0.03}$ | $3422^{+17}_{-49}$ |  BPRP inter
3872 B | 162.38755782729 | 27.19025918622 | $5.80^{+0.21}_{-0.32}$ | 938 | $0.74^{+0.05}_{-0.05}$ | $5392^{+348}_{-331}$ |  PRI BPRP
3875 B | 204.08561299815 | 68.52200415724 | $5.38^{+0.46}_{-0.30}$ | 7220 | $0.87^{+0.05}_{-0.03}$ | $5228^{+337}_{-110}$ |  PRI BPRP NSS
3883 B | 183.96410252047 | 47.42821260192 | $8.40^{+0.41}_{-0.30}$ | 2601 | $0.64^{+0.01}_{-0.01}$ | $3817^{+24}_{-23}$ | BPRP
3889 B | 180.25780661146 | 55.84614755703 | $6.80^{+0.50}_{-0.53}$ | 698 | $0.70^{+0.04}_{-0.01}$ | $4586^{+125}_{-105}$ |  PRI BPRP

Table 5: continued

TOI | $\alpha$ | $\delta$ | $M_{\rm G}$ | $sep$ | $mass$ | $T_{\rm eff}$ | Flags
---|---|---|---|---|---|---|---
| [∘] | [∘] | [mag] | [au] | [$M_{\odot}$] | [K] |
3896 B | 187.93969685290 | 63.90585576769 | $9.41^{+0.14}_{-0.19}$ | 3274 | $0.45^{+0.01}_{-0.01}$ | $3480^{+22}_{-61}$ |  PRI BPRP
3915 B | 205.48821304826 | 17.30005590348 | $10.97^{+0.03}_{-0.05}$ | 476 | $0.25^{+0.14}_{-0.10}$ | $3268^{+316}_{-282}$ |
3920 B | 336.69063547736 | 57.43370262278 | $7.71^{+0.32}_{-0.25}$ | 841 | $0.58^{+0.18}_{-0.17}$ | $4162^{+1009}_{-616}$ |
3922 A | 228.83275054542 | 40.26678851965 | $4.80^{+0.10}_{-0.10}$ | 550 | $0.90^{+0.06}_{-0.07}$ | $5904^{+295}_{-296}$ |  PRI BPRP
3956 A | 229.21827948120 | 51.39777270307 | $3.93^{+0.15}_{-0.25}$ | 1760 | $0.98^{+0.12}_{-0.09}$ | $5979^{+361}_{-280}$ |  PRI BPRP NSS
3966 B | 225.38169817837 | 38.53370077153 | $10.10^{+0.17}_{-0.23}$ | 828 | $0.36^{+0.02}_{-0.02}$ | $3420^{+29}_{-33}$ |  BPRP inter
3977 B | 231.12743053572 | 46.69506834347 | $5.65^{+0.18}_{-0.38}$ | 659 | $0.74^{+0.04}_{-0.04}$ | $5616^{+255}_{-322}$ |  PRI BPRP
3984 B | 226.33680816581 | 36.78784975544 | $13.68^{+0.16}_{-0.16}$ | 356 |  |  |  BPRP WD
3998 B | 7.63787900943 | 56.33181795423 | $9.38^{+0.02}_{-0.23}$ | 885 | $0.42^{+0.17}_{-0.15}$ | $3606^{+542}_{-343}$ | BPRP
4001 B | 2.52363216857 | 64.57429750735 | $6.18^{+0.04}_{-0.19}$ | 3245 | $0.77^{+0.03}_{-0.04}$ | $4891^{+200}_{-132}$ |  PRI BPRP
4021 B | 28.65074517816 | 64.56885859645 | $5.98^{+0.29}_{-0.25}$ | 5639 | $0.79^{+0.02}_{-0.05}$ | $5071^{+584}_{-228}$ |  PRI BPRP
4040 B | 268.61512748281 | 77.48923373608 | $13.01^{+0.07}_{-0.15}$ | 989 | $0.14^{+0.01}_{-0.01}$ | $2979^{+22}_{-10}$ |  BPRP inter
4059 B | 274.18010202664 | 76.89014057693 | $8.25^{+0.11}_{-0.19}$ | 1199 | $0.45^{+0.01}_{-0.01}$ | $4265^{+219}_{-439}$ | BPRP
4070 A | 250.27677877596 | 42.43723126784 | $3.95^{+0.07}_{-0.19}$ | 1532 | $0.99^{+0.13}_{-0.10}$ | $6316^{+362}_{-305}$ |  PRI BPRP
4077 B | 250.30191634926 | 38.96497231403 | $10.53^{+0.11}_{-0.20}$ | 4731 | $0.35^{+0.01}_{-0.01}$ | $3256^{+4}_{-3}$ |  BPRP SHC2
4079 A | 19.97560713621 | 64.53580319915 | $3.51^{+0.18}_{-0.18}$ | 4168 | $1.20^{+0.09}_{-0.14}$ | $6660^{+436}_{-382}$ |  PRI BPRP
4081 B | 21.57135203059 | 64.83988013998 | $5.17^{+0.35}_{-0.35}$ | 980 | $0.93^{+0.05}_{-0.05}$ | $5450^{+200}_{-163}$ |  BPRP inter
4089 B | 267.85149807828 | 22.66149859234 | $5.84^{+0.02}_{-0.51}$ | 426 | $0.77^{+0.21}_{-0.18}$ | $5237^{+834}_{-1058}$ |
4107 B | 269.24657644488 | 58.88101313795 | $8.78^{+0.13}_{-0.35}$ | 1898 | $0.55^{+0.01}_{-0.01}$ | $3584^{+51}_{-31}$ | BPRP
4113 B | 283.89266583485 | 71.40095184180 | $11.54^{+0.02}_{-0.27}$ | 531 | $0.21^{+0.01}_{-0.01}$ | $3170^{+33}_{-3}$ |  BPRP inter
4123 B | 131.23352602350 | 75.10638543419 | $10.90^{+0.07}_{-0.08}$ | 620 | $0.27^{+0.01}_{-0.01}$ | $3265^{+15}_{-12}$ |  BPRP inter
4128 B | 128.23671176505 | 82.03039044190 | $6.08^{+0.19}_{-0.21}$ | 7354 | $0.79^{+0.06}_{-0.04}$ | $4946^{+191}_{-177}$ |  PRI BPRP NSS
4145 B | 39.43164905049 | 80.26774459975 | $11.34^{+0.09}_{-0.17}$ | 356 | $0.21^{+0.14}_{-0.07}$ | $3173^{+302}_{-289}$ |
4168 B | 173.82185450357 | 79.41401164812 | $6.91^{+0.13}_{-0.22}$ | 2804 | $0.70^{+0.04}_{-0.01}$ | $4443^{+144}_{-121}$ |  PRI BPRP
4175 B | 198.53969402570 | -16.55942836813 | $4.58^{+0.21}_{-0.21}$ | 75 | $0.95^{+0.09}_{-0.09}$ | $6082^{+294}_{-268}$ | BPRP
4175 C | 198.54163019207 | -16.60566374031 | $10.44^{+0.05}_{-0.29}$ | 7727 | $0.35^{+0.01}_{-0.01}$ | $3240^{+15}_{-44}$ |  PRI BPRP
4176 B | 201.99815807515 | -29.78494557416 | $5.82^{+0.03}_{-0.19}$ | 9366 | $0.74^{+0.03}_{-0.04}$ | $5351^{+166}_{-168}$ |  PRI BPRP
4179 A | 202.41900469667 | -16.56534510191 | $4.74^{+0.08}_{-0.21}$ | 3615 | $0.94^{+0.06}_{-0.09}$ | $5882^{+248}_{-242}$ |  PRI BPRP
4182 B | 45.90781719137 | -69.74348706667 | $10.93^{+0.02}_{-0.19}$ | 2315 | $0.25^{+0.01}_{-0.01}$ | $3278^{+11}_{-61}$ |  PRI BPRP
4192 B | 23.78717048262 | -41.50697537823 | $5.49^{+0.13}_{-0.12}$ | 1332 | $0.75^{+0.05}_{-0.04}$ | $5702^{+275}_{-326}$ |  PRI BPRP
4212 B | 116.38141838603 | -25.99214271609 | $12.72^{+0.32}_{-0.32}$ | 7221 | $0.15^{+0.01}_{-0.01}$ | $3021^{+45}_{-46}$ |
4226 B | 116.96489620573 | -25.56643169835 | $11.08^{+0.44}_{-0.46}$ | 2226 | $0.25^{+0.06}_{-0.03}$ | $3233^{+86}_{-60}$ |  BPRP inter
4245 B | 125.80648008533 | -45.79287939591 | $10.65^{+0.16}_{-0.30}$ | 346 | $0.30^{+0.14}_{-0.11}$ | $3325^{+313}_{-268}$ |
4293 B | 302.97797038614 | -49.00095806061 | $9.40^{+0.11}_{-0.18}$ | 1170 | $0.43^{+0.02}_{-0.01}$ | $3534^{+40}_{-26}$ |  BPRP inter
4301 B | 166.26442627031 | -46.03699476689 | $13.21^{+0.08}_{-0.10}$ | 4984 |  |  | WD
4303 B | 72.35767076023 | -43.35604073937 | $7.86^{+0.18}_{-0.32}$ | 2309 | $0.60^{+0.01}_{-0.01}$ | $3992^{+121}_{-73}$ |  PRI BPRP
4325 B | 101.84813744489 | 6.13570650776 | $11.87^{+0.26}_{-0.20}$ | 1296 | $0.22^{+0.01}_{-0.01}$ | $2972^{+8}_{-51}$ |  PRI BPRP
4330 B | 220.35023214342 | -33.94988039998 | $4.25^{+0.02}_{-0.29}$ | 628 | $0.96^{+0.29}_{-0.16}$ | $5943^{+779}_{-559}$ |
4337 A | 164.28776576746 | -69.98061944588 | $4.89^{+0.06}_{-0.18}$ | 332 | $0.94^{+0.06}_{-0.06}$ | $5619^{+236}_{-211}$ |  PRI BPRP
4339 A | 212.92908519599 | -29.97493629373 | $8.51^{+0.16}_{-0.36}$ | 448 | $0.55^{+0.01}_{-0.01}$ | $3728^{+30}_{-27}$ |  PRI BPRP
4344 B | 69.64989596367 | -61.34368885093 | $9.32^{+0.01}_{-0.17}$ | 486 | $0.42^{+0.18}_{-0.15}$ | $3627^{+618}_{-354}$ |
4349 B | 0.12979485849 | -26.23033985535 | $10.25^{+0.27}_{-0.30}$ | 193 | $0.30^{+0.01}_{-0.05}$ | $3475^{+65}_{-191}$ | BPRP

Table 5: continued

TOI | $\alpha$ | $\delta$ | $M_{\rm G}$ | $sep$ | $mass$ | $T_{\rm eff}$ | Flags
---|---|---|---|---|---|---|---
| [∘] | [∘] | [mag] | [au] | [$M_{\odot}$] | [K] |
4350 B | 32.88391134546 | -76.10637329379 | $9.52^{+0.11}_{-0.17}$ | 393 | $0.41^{+0.05}_{-0.02}$ | $3489^{+139}_{-128}$ | BPRP
4359 B | 149.73699892763 | -53.30425173334 | $9.37^{+0.14}_{-0.16}$ | 2728 | $0.45^{+0.01}_{-0.01}$ | $3497^{+64}_{-64}$ |  PRI BPRP
4366 B | 180.29004388300 | -67.75581738345 | $7.53^{+0.46}_{-0.38}$ | 4870 | $0.60^{+0.01}_{-0.01}$ | $4133^{+135}_{-65}$ |  PRI BPRP
4369 B | 100.58750610095 | -58.18153364282 | $2.94^{+0.17}_{-0.17}$ | 1736 | $1.31^{+0.12}_{-0.22}$ | $6369^{+420}_{-469}$ |  PRI BPRP
4370 B | 201.46970099045 | -16.42600768553 | $9.90^{+0.03}_{-0.05}$ | 6604 | $0.40^{+0.01}_{-0.01}$ | $3381^{+74}_{-55}$ |  PRI BPRP
4372 B | 218.85166922760 | -76.21442871924 | $12.32^{+0.14}_{-0.26}$ | 629 | $0.17^{+0.01}_{-0.01}$ | $3076^{+32}_{-17}$ |  BPRP inter
4390 B | 262.64794769062 | -52.33654991895 | $3.36^{+0.18}_{-0.18}$ | 212 | $1.30^{+0.05}_{-0.05}$ | $6483^{+127}_{-120}$ |  BPRP inter
4414 A | 267.47501105883 | -37.53114551499 | $2.25^{+0.04}_{-0.04}$ | 291 | $1.80^{+0.02}_{-0.01}$ | $7633^{+85}_{-81}$ | inter
4420 B | 246.80051205533 | -69.34279402648 | $6.07^{+0.18}_{-0.15}$ | 1062 | $0.85^{+0.01}_{-0.01}$ | $4898^{+159}_{-29}$ |  PRI BPRP SHC2 NSS
4425 B | 264.84072608556 | -35.39308157571 | $8.84^{+0.21}_{-0.24}$ | 879 | $0.49^{+0.01}_{-0.01}$ | $3732^{+29}_{-23}$ |  BPRP SHC2
4463 B | 279.36130629852 | 18.72900308391 | $10.14^{+0.20}_{-0.21}$ | 2009 | $0.40^{+0.01}_{-0.01}$ | $3271^{+10}_{-9}$ |  PRI BPRP
4499 B | 284.36118628028 | 39.07217949918 | $11.35^{+0.08}_{-0.10}$ | 2566 | $0.27^{+0.01}_{-0.01}$ | $3023^{+8}_{-6}$ | BPRP
4522 B | 23.30225457564 | 5.64522664713 | $11.30^{+0.11}_{-0.11}$ | 1589 | $0.23^{+0.01}_{-0.01}$ | $3199^{+14}_{-13}$ |  BPRP inter
4546 A | 51.43958735455 | 23.18677535559 | $2.03^{+0.27}_{-0.27}$ | 2478 | $1.61^{+0.22}_{-0.17}$ | $7354^{+703}_{-587}$ |  PRI BPRP

Table 5: continued

CTOI | $\alpha$ | $\delta$ | $M_{\rm G}$ | $sep$ | $mass$ | $T_{\rm eff}$ | Flags
---|---|---|---|---|---|---|---
| [∘] | [∘] | [mag] | [au] | [$M_{\odot}$] | [K] |
13073396 B | 348.05671579910 | -27.36857356304 | $12.25^{+0.08}_{-0.07}$ | 4961 |  |  |  BPRP WD
37652870 B | 2.18607214877 | -7.85952561311 | $11.30^{+0.22}_{-0.15}$ | 5393 | $0.25^{+0.01}_{-0.01}$ | $3110^{+54}_{-8}$ |  PRI BPRP
94984950 B | 250.46683181731 | -32.80896712763 | $12.46^{+0.23}_{-0.21}$ | 2212 | $0.16^{+0.01}_{-0.01}$ | $3059^{+26}_{-33}$ |  BPRP inter
145601161 B | 132.53210895700 | -50.58986267488 | $9.36^{+0.35}_{-0.57}$ | 2885 | $0.30^{+0.07}_{-0.01}$ | $3404^{+50}_{-66}$ |  PRI BPRP