# VaTEST II: Statistical Validation of 16 Exoplanets of TESS

Priyashkumar Mistry Department of Physics, Sardar Vallabhbhai National
Institute of Technology, Surat-395007, Gujarat, India  Kamlesh Pathak
Department of Physics, Sardar Vallabhbhai National Institute of Technology,
Surat-395007, Gujarat, India  Aniket Prasad Department of Physics, National
Institute of Technology Agartala 799046, Tripura, India  Georgios Lekkas
Department of Physics, University of Ioannina, Ioannina, 45110, Greece
Surendra Bhattarai Department of Physics, Indian Institute of Science
Education and Research Kolkata, Mohanpur-741246, West Bengal, India  Sarvesh
Gharat Centre for Machine Intelligence and Data Science, Indian Institute of
Technology Bombay  Mousam Maity Department of Physics, Presidency University,
Kolkata-700073, West Bengal, India  Dhruv Kumar Department of Physics,
National Institute of Technology Agartala 799046, Tripura, India  Elise Furan
NASA Exoplanet Science Institute, Caltech/IPAC, Mail Code 100-22, 1200 E.
California Blvd., Pasadena, CA 91125, USA  Steve Howell NASA Ames Research
Center, Moffett Field, CA 94035, USA  David Ciardi NASA Exoplanet Science
Institute, Caltech/IPAC, Mail Code 100-22, 1200 E. California Blvd., Pasadena,
CA 91125, USA  Allyson Bieryla Center for Astrophysics, Harvard & Smithsonian,
60 Garden St, Cambridge, MA 02138, USA  Elisabeth Matthews Max-Planck-Institut
für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany  Erica Gonzales
Department of Astronomy and Astrophysics, University of California Santa Cruz,
Santa Cruz, CA 95064, USA  Carl Ziegler Department of Physics, Engineering and
Astronomy, Stephen F. Austin State University, 1936 North St, Nacogdoches, TX
75962, USA  Ian Crossfield Department of Physics & Astronomy, University of
Kansas, KS 66045, USA  Jason Eastman Center for Astrophysics, Harvard &
Smithsonian, 60 Garden St, Cambridge, MA 02138, USA  Steven Giacalone
Department of Astronomy, University of California Berkeley, Berkeley, CA
94720, USA  Courtney Dressing Department of Astronomy, University of
California Berkeley, Berkeley, CA 94720, USA  Charles Beichman NASA Exoplanet
Science Institute, Caltech/IPAC, Mail Code 100-22, 1200 E. California Blvd.,
Pasadena, CA 91125, USA  Abderahmane Soubkiou Oukaimeden Observatory, High
Energy Physics and Astrophysics Laboratory, Cadi Ayyad University, Marrakech,
Morocco  Zouhair Benkhaldoun Oukaimeden Observatory, High Energy Physics and
Astrophysics Laboratory, Cadi Ayyad University, Marrakech, Morocco  Joshua
Schlieder NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD
20771, USA  Maria V. Goliguzova Sternberg Astronomical Institute, M.V.
Lomonosov Moscow State University, 13, Universitetskii pr., 119234, Moscow,
Russia  Ivan A. Strakhov Sternberg Astronomical Institute, M.V. Lomonosov
Moscow State University, 13, Universitetskii pr., 119234, Moscow, Russia  Mark
Everett NSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N.
Cherry Ave., Tucson, AZ 85719, USA  Crystal Gnilka NASA Ames Research Center,
Moffett Field, CA 94035, USA  Katie Lester NASA Ames Research Center, Moffett
Field, CA 94035, USA  Colin Littlefield NASA Ames Research Center, Moffett
Field, CA 94035, USA  Bay Area Environmental Research Institute, Moffett
Field, CA 94035, USA  Nic Scott NASA Ames Research Center, Moffett Field, CA
94035, USA  Rachel Matson NASA Ames Research Center, Moffett Field, CA 94035,
USA

###### Abstract

NASA’s Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey
mission designed to find transiting exoplanets orbiting near bright stars. It
has identified more than 250 transiting exoplanets, and almost 6,000
candidates are yet to be studied. In this manuscript, we discuss the findings
from the ongoing VaTEST (Validation of Transiting Exoplanets using Statistical
Tools) project, which aims to validate new exoplanets for further
characterization. We validated 16 new exoplanets by examining the light curves
of 30 candidates using LATTE tool and computing the False Positive
Probabilities using multiple statistical validation tools like VESPA and
TRICERATOPS. These include planets suitable for atmospheric characterization
using transmission spectroscopy (TOI-2194b), emission spectroscopy (TOI-277b,
TOI-1853b and TOI-3082b) and for both transmission and emission spectroscopy
(TOI-672b, TOI-1410b, TOI-1694b, TOI-2018b, TOI-2134b and TOI-2443b); Two
super-Earths (TOI-1801b and TOI-2194b) orbiting bright (V = 11.58 mag, V =
8.42 mag), metal-poor ([Fe/H] = -0.7186 $\pm$ 0.1, [Fe/H] = -0.3720 $\pm$ 0.1)
stars; two short-period Neptune like planets (TOI-1410b and TOI-1853b) in Hot
Neptune Desert. In total, we validated 2 super-Earths, 9 sub-Neptunes, 3
Neptune-like, and 2 sub-Saturn or super-Neptune-like exoplanets. Additionally,
we identify three more candidates (TOI-1732, TOI-2200, and TOI-5704) which can
be further studied to establish their planetary nature.

methods: statistical — techniques: photometric

††journal: AJ††software: TLS (Hippke & Heller, 2019), Lightkurve (Lightkurve
Collaboration et al., 2018), Juliet (Espinoza et al., 2019), VESPA (Morton,
2012) and TRICERATOPS (Giacalone & Dressing, 2020).

##  1 Introduction

The Transiting Exoplanet Survey Satellite (TESS) (Ricker et al., 2010) mission
is an all-sky survey to discover exoplanets in nearby regions. It was launched
on April 18, 2018 aboard a SpaceX Falcon 9 rocket. During its two-year study,
the TESS spacecraft concentrated on nearby G, K, and M type stars with
apparent magnitudes $<$ 12\. An area 400 times greater than the one covered by
the Kepler campaign was to be surveyed, including the 1,000 nearest dwarf
stars in the entire sky. More than 3000 transiting exoplanets, including
500–1000 Earth-sized planets and large planets, were anticipated to be
discovered by TESS. The survey was divided into 26 viewing zones called
sectors, each of which was 24${\arcdeg}$ $\times$ 96${\arcdeg}$. The
spacecraft had spent two 13.7 days orbiting each sector, mapping the southern
hemisphere in its first year of operation and the northern hemisphere in its
second year. TESS’s primary mission (cycles 1 and 2, sectors 1–26) was
completed in July 2020. The first extended mission (cycles 3 and 4, sectors
27–55) ended in September 2022, and it is now on its second extended mission
(cycle 5, sectors 56–69).

We currently have 282 confirmed TESS exoplanets and 6119 TESS
candidates111https://exoplanetarchive.ipac.caltech.edu/, accessed on December
16, 2022 that need to be studied. By using the conventional method, i.e., a
combination of transit and radial velocity to discover a new planet, it is
very difficult to study this large number of candidates. There are so-called
astrophysical false positives (Cameron, 2012), such as eclipsing binaries,
blended eclipsing binaries, and planet-sized stars in binary systems, that can
generate a transit-like signal. Many tools have been developed based on
transit photometry to calculate their likelihood and probability of being
planets or false positives. To rule out false positives, BLENDER (Torres et
al., 2010) was the first approach based on $\chi^{2}$ statistics on eclipsing
binaries and blended eclipsing binaries. VESPA (Morton, 2015) was another
approach that used the MCMC sampling routine to fit the Kepler light curve and
produced a false-positive probability based on the fit. Both VESPA and BLENDER
can account for subsequent high-contrast imaging. The framework was widely
used to statistically validate exoplanets from Kepler as well as TESS. The
another robust model PASTIS (Díaz et al., 2014) which can take transit
photometry data as well as high precision radial velocity measurements to
validate the planet. Alternatively, TRICERATOPS (Giacalone & Dressing, 2020)
was specifically developed to take advantage of the unique features and
requirements of the TESS mission. With a lower resolution than previous such
missions, there is an even greater necessity to account for multiple star
systems and scenarios like diluted transits. Such approaches can be used to
validate new exoplanets in bulk without having radial velocity measurements.
For our project, we made use of VESPA and TRICERATOPS as independent
validation tools to calculate the FPP of selected candidates.

The Validation of Transiting Exoplanets using Statistical Tools (VaTEST)
project222https://sites.google.com/view/project-vatest/home has its primary
goal to validate bulk exoplanets with the use of various statistical
validation approaches. In our first paper, we discovered our first planet,
TOI-181b (Mistry et al., 2022), by utilising a similar approach. For the
future, we have separated candidates based on their spectral types
(temperatures) and will study them each individually in order to find out
their planetary nature. However, for this manuscript, we will validate the
exoplanets orbiting K-type (temperature range 3700–5200 K, (Habets & Heintze,
1981; Weidner & Vink, 2010) stars. Here we validated a significant number of
exoplanets from the candidates observed by TESS.

This paper is structured as follows: In section 2 we discuss our methodology
to select the most promising candidates for the validation process, and in
section 3 we present the follow-up observation that is used during the
calculation of FPP. The algorithm and procedure for using the statistical
validation tools VESPA and TRICERATOPS are covered in Section 4. In section 5
we presented the main features of newly validated systems. Finally, section 6
describes not validated candidates and some likely planets that can be
followed up further to validate.

##  2 Selection of Candidates

In this manuscript, we study planets orbiting K spectral type stars. There
were multiple restrictions made while selecting the targets for our study,
such as:

  * •

Reported orbital period $<20$ days

  * •

Planetary radii $<8\text{R}_{E}$

  * •

Removed targets with the dispositions CP (Confirmed Planet), KP (Known
Planet), FP (False Positive) and EB (Eclipsing Binary)

As we have used only the transit photometry data for confirming the
exoplanetary nature of a signal, it is imperative to have a maximum number of
transits present in the light curve. The minimum number of transits required
to confirm the existence of an exoplanet is typically at least three. For this
reason we choose targets showing $<20$ days orbital period. The major reason
behind having radii $<8\text{R}_{E}$ is the statistical validation tool called
TRICERATOPS (Giacalone & Dressing, 2020). TRICERATOPS under-predicts the false
positive probability for planetary candidates having radii $\geq
8\text{R}_{E}$.

A total of 343 candidates from the ExoFOP TESS Object of Interest (TOI)
database333https://exofop.ipac.caltech.edu/tess are considered in this study.
To identify probable binary stars, use of Renormalized Unit Weight Error
(RUWE) score (Lindegren et al., 2018; Belokurov et al., 2020) from Gaia EDR3
is done. Targets with an RUWE score of $\geq 1.4$ or null (David et al., 2021)
are eliminated. Additionally, targets with stellar companions, lacking SPOC
pipeline data, or without available stellar parameters were also excluded from
this study. A visual inspection of the remaining targets was performed to
eliminate any signals that were consistent with star variability, eclipsing
binaries, or instrumental systematic effects. Finally, the use of Juliet
modeling (Espinoza et al., 2019) is done on the remaining set of targets to
identify eclipsing binaries based on the characteristics of transit light
curves. Through this initial screening process, a total of 30 significant
objects were identified for further examination of their planetary nature.
Stellar parameters for these selected targets are shown in Table 1.

Prior to conducting probabilistic analysis, it is essential to verify the
origin of the generated signal. To accomplish this, we employed the Lightcurve
Analysis Tool for Transiting Exoplanet (LATTE) as described in (Eisner et al.,
2020). The results of the LATTE tests for all of the considered candidates
have been uploaded to a publicly available GitHub
repository444https://github.com/priyashmistry/VaTEST-II-Output-Files.git for
further examination. This step serves as a crucial initial check to ensure
that the signals under investigation are indeed emanating from the target
sources, thereby providing a necessary foundation for subsequent probabilistic
analysis.

Table 1: Stellar parameters of the candidate systems.  No. | TOI ID | TIC ID | T${}_{e}ff$ | Rs | Ms | logg | [Fe/H] | V | TESS | RUWE
---|---|---|---|---|---|---|---|---|---|---
|  |  | [K] | [$R_{\sun}$] | [$M_{\sun}$] |  | [dex] | [mag] | [mag] |
1 | TOI 139 | 62483237 | 4570 $\pm$ 50 | 0.7007 $\pm$ 0.0575 | 0.6900 $\pm$ 0.0852 | 4.705 $\pm$ 0.100 | -0.238 $\pm$ 0.080 | 10.55 | 9.36 | 0.8818
2 | TOI 277 | 439456714 | 3748 $\pm$ 64 | 0.5231 $\pm$ 0.0156 | 0.5204 $\pm$ 0.0203 | 4.785 $\pm$ 0.029 | -0.630 $\pm$ 0.585 | 13.63 | 11.73 | 1.2830
3 | TOI 323 | 251852984 | 4558 $\pm$ 122 | 0.7756 $\pm$ 0.1000 | 0.7370 $\pm$ 0.0455 | 4.613 $\pm$ 0.027 | -0.040 $\pm$ 0.325 | 14.35 | 13.35 | 1.0132
4 | TOI 493 | 19025965 | 4402 $\pm$ 100 | 0.8119 $\pm$ 0.0661 | 0.6480 $\pm$ 0.0829 | 4.689 $\pm$ 0.100 | -0.181 $\pm$ 0.080 | 12.55 | 11.45 | 1.1079
5 | TOI 672 | 151825527 | 3765 $\pm$ 65 | 0.5441 $\pm$ 0.0163 | 0.5399 $\pm$ 0.0204 | 4.699 $\pm$ 0.010 | -0.710 $\pm$ 0.625 | 13.58 | 11.67 | 1.1587
6 | TOI 815 | 102840239 | 4954 $\pm$ 107 | 0.7594 $\pm$ 0.0426 | 0.8200 $\pm$ 0.0943 | 4.591 $\pm$ 0.081 | 0.037 $\pm$ 0.039 | 10.22 | 9.36 | 1.0129
7 | TOI 913 | 407126408 | 4969 $\pm$ 129 | 0.7325 $\pm$ 0.0488 | 0.8200 $\pm$ 0.0973 | 4.622 $\pm$ 0.089 | -0.133 $\pm$ 0.100 | 10.45 | 9.62 | 1.0136
8 | TOI 1179 | 148914726 | 4998 $\pm$ 50 | 0.7770 $\pm$ 0.0110 | 0.8050 $\pm$ 0.4450 | 4.462 $\pm$ 0.100 | -0.084 $\pm$ 0.080 | 10.88 | 10.13 | 1.0336
9 | TOI 1180 | 158002130 | 4900 $\pm$ 50 | 0.7272 $\pm$ 0.0518 | 0.7500 $\pm$ 0.0934 | 4.723 $\pm$ 0.100 | -0.024 $\pm$ 0.080 | 11.02 | 10.11 | 0.9415
10 | TOI 1410 | 199444169 | 4668 $\pm$ 50 | 0.7787 $\pm$ 0.0618 | 0.7960 $\pm$ 0.0370 | 4.582 $\pm$ 0.100 | 0.066 $\pm$ 0.080 | 11.11 | 10.19 | 1.1397
11 | TOI 1694 | 396740648 | 5135 $\pm$ 50 | 0.8183 $\pm$ 0.0477 | 0.8450 $\pm$ 0.1089 | 4.658 $\pm$ 0.100 | 0.060 $\pm$ 0.080 | 11.45 | 10.74 | 1.3827
12 | TOI 1732 | 470987100 | 3876 $\pm$ 157 | 0.6326 $\pm$ 0.0187 | 0.6139 $\pm$ 0.0203 | 4.624 $\pm$ 0.011 | 0.291 $\pm$ 0.100 | 12.89 | 11.33 | 1.3104
13 | TOI 1801 | 119584412 | 3815 $\pm$ 157 | 0.5456 $\pm$ 0.0164 | 0.5413 $\pm$ 0.0204 | 4.698 $\pm$ 0.010 | -0.719 $\pm$ 0.100 | 11.58 | 9.86 | 1.0407
14 | TOI 1853 | 73540072 | 5175 $\pm$ 50 | 0.8397 $\pm$ 0.0474 | 0.8200 $\pm$ 0.0992 | 4.630 $\pm$ 0.100 | 0.285 $\pm$ 0.080 | 12.18 | 11.37 | 1.0895
15 | TOI 2018 | 357501308 | 4348 $\pm$ 100 | 0.6225 $\pm$ 0.0766 | 0.6600 $\pm$ 0.0868 | 4.733 $\pm$ 0.100 | -0.633 $\pm$ 0.080 | 10.25 | 8.96 | 1.2333
16 | TOI 2134 | 75878355 | 4569 $\pm$ 50 | 0.7697 $\pm$ 0.0640 | 0.6900 $\pm$ 0.0791 | 4.610 $\pm$ 0.100 | - | 8.93 | 7.79 | 1.0239
17 | TOI 2194 | 271478281 | 4756 $\pm$ 50 | 0.6909 $\pm$ 0.0492 | 0.7400 $\pm$ 0.0854 | 4.698 $\pm$ 0.100 | -0.372 $\pm$ 0.100 | 8.42 | 7.43 | 0.9936
18 | TOI 2200 | 142105158 | 5070 $\pm$ 117 | 0.8262 $\pm$ 0.0487 | 0.8500 $\pm$ 0.1038 | 4.533 $\pm$ 0.084 | 0.273 $\pm$ 0.100 | 13.09 | 12.32 | 1.0810
19 | TOI 2408 | 67630845 | 4935 $\pm$ 132 | 0.7485 $\pm$ 0.0510 | 0.8100 $\pm$ 0.0969 | 4.598 $\pm$ 0.092 | - | 12.78 | 11.92 | 1.0093
20 | TOI 2443 | 318753380 | 4357 $\pm$ 100 | 0.7321 $\pm$ 0.0713 | 0.6600 $\pm$ 0.0789 | 4.709 $\pm$ 0.100 | -0.439 $\pm$ 0.080 | 9.51 | 8.30 | 1.2536
21 | TOI 2459 | 192790476 | 4195 $\pm$ 124 | 0.6751 $\pm$ 0.0630 | 0.6600 $\pm$ 0.0763 | 4.599 $\pm$ 0.107 | - | 10.77 | 9.40 | 1.1358
22 | TOI 3082 | 428699140 | 4263 $\pm$ 100 | 0.6847 $\pm$ 0.0613 | 0.6640 $\pm$ 0.0798 | 4.625 $\pm$ 0.100 | 0.170 $\pm$ 0.080 | 12.93 | 11.77 | 1.2058
23 | TOI 3568 | 160390955 | 4890 $\pm$ 50 | 0.7858 $\pm$ 0.0517 | 0.7920 $\pm$ 0.0942 | 4.540 $\pm$ 0.100 | 0.002 $\pm$ 0.080 | 12.88 | 12.07 | 0.9779
24 | TOI 3896 | 445837596 | 5043 $\pm$ 50 | 0.7478 $\pm$ 0.0431 | 0.8600 $\pm$ 0.1032 | 4.419 $\pm$ 0.100 | -0.279 $\pm$ 0.080 | 12.43 | 11.68 | 0.9606
25 | TOI 3913 | 155898758 | 4180 $\pm$ 123 | 0.8257 $\pm$ 0.0767 | 0.6540 $\pm$ 0.0813 | 4.420 $\pm$ 0.110 | 0.137 $\pm$ 0.110 | 13.71 | 12.58 | 1.0625
26 | TOI 4090 | 289373041 | 4740 $\pm$ 124 | 0.8194 $\pm$ 0.0567 | 0.7600 $\pm$ 0.0909 | 4.492 $\pm$ 0.095 | 0.760 $\pm$ 0.091 | 13.40 | 12.55 | 1.0152
27 | TOI 4308 | 144193715 | 5243 $\pm$ 126 | 0.7934 $\pm$ 0.0465 | 0.9000 $\pm$ 0.1133 | 4.593 $\pm$ 0.087 | - | 11.25 | 10.34 | 0.8720
28 | TOI 5584 | 29169215 | 4372 $\pm$ 100 | 0.7451 $\pm$ 0.0684 | 0.6400 $\pm$ 0.0789 | 4.725 $\pm$ 0.100 | 0.128 $\pm$ 0.065 | 11.83 | 10.73 | 1.0809
29 | TOI 5704 | 148673433 | 4590 $\pm$ 126 | 0.7575 $\pm$ 0.0593 | 0.7300 $\pm$ 0.0846 | 4.543 $\pm$ 0.095 | 0.428 $\pm$ 0.100 | 11.53 | 10.61 | 1.2287
30 | TOI 5803 | 466382581 | 5134 $\pm$ 121 | 0.7625 $\pm$ 0.0451 | 0.8700 $\pm$ 0.1032 | 4.613 $\pm$ 0.085 | - | 10.66 | 9.94 | 0.9834

##  3 Follow-up Observation

###  3.1 Speckle Imaging

Speckle imaging was observed using ’Alopeke and Zorro instrument installed on
Gemini 8m telescope, HRCam instrument on the SOAR 4.1m telescope and Speckle
Polarimeter on SAI 2.5m telescope. The Differential Speckle Survey Instrument-
based (DSSI, Horch et al. (2009)) imagers ’Alopeke and Zorro are identical
fast, low-noise, dual-channel, and dual-plate-scale imagers. ’Alopeke and
Zorro are permanently installed at the calibration ports at Gemini North and
South, respectively. They offer simultaneous two-color (red and blue)
diffraction-limited optical imaging (FWHM 0.02$\arcsec$ at 650nm) in speckle
mode over a 6.7$\arcsec$ field of view for targets as dim as V 17. Data is
collected as a time series of 1000 images with an exposure time of 60 ms on a
256 $\times$ 256 pixel sub-array covering a 2.5$\arcsec$ region of the sky. A
high-resolution camera (HRCam) that can observe the $9.9\arcsec\times
7.5\arcsec$ field of the sky has a 658 $\times$ 496 pixel array, with each
pixel able to collect light from a 15 mas region (Tokovinin et al., 2010). It
is a fast imager designed to work at the SOAR telescope, which uses a CCD
detector with internal electro-multiplication (EMCCD). HRCam consists of the
detector, mechanical structure, filter wheel, and optics. SOAR’s f/16 beam is
collimated by a 50-mm negative achromat (Barlow lens) and refocused by a 100mm
positive lens, effectively doubling the telescope focal length and providing a
pixel scale of 15 mas. The 2.5m CO SAI MSU (Caucasian Observatory of the
Sternberg Astronomical Institute of Lomonosov Moscow State University)
telescope’s speckle polarimeter (Safonov et al., 2017) is a facility
instrument that studies the spatial structure and polarisation of
astrophysical objects at diffraction-limited resolutions between 400 and 1100
nm. It is a two-beam polarimeter with a half-wave plate and a speckle
interferometer. The detector is a quick electron-multiplying CCD. Field of
View (FoV) for this instrument is $5\arcsec\times 10\arcsec$.

###  3.2 Adaptive Optics Imaging

Data for the Adaptive Optics (AO) imaging was collected from NIRI (Near
Infrared Imager) installed on the Gemini 8m telescope, NIRC2 on the Keck 10m
telescope, PHARO (Palomar High Angular Resolution Observer) on 200-inch Hale
telescope at Palomar Observatory, ShARCS (Shane Adaptive optics infraRed
Camera-Spectrograph) on Lick Observatory’s 3-m Shane telescope and NaCo
(Nasmyth Adaptive Optics System (NAOS) – Near-Infrared Imager and Spectrograph
(CONICA)) installed on the Very Large Telescope (VLT). The primary NIR imager
at Gemini North is NIRI (Hodapp et al., 2003). It features three cameras and a
broad selection of wide- and narrow-band filters. It is possible to employ
NIRI f/32 (FoV $22\arcsec\times 22\arcsec$) for J-L’ imaging and NIRI f/14
(FoV $51\arcsec\times 51\arcsec$) for imaging out to 2.5 microns with the
Gemini facility adaptive optics (AO) system, ALTAIR (either with a natural
guide star or the laser guide star). The benefit of AO at L’ is negligible and
only applies to point sources. A near-infrared imager called NIRC2 was created
for the Keck system of adaptive optics. NIRC2 (Lu et al., 2016) is situated on
Keck II’s left Nasmyth Platform, behind the AO bench. The instrument has three
configurable cameras with pixel scales of 10, 20, and 40 mas/pixel to
accommodate the expected range in image sizes. The instrument operates from 1
to 5 microns. A focal plane mechanism provides slits and occulting areas for
coronography, and two filter wheels with 18 positions each provide a range of
filters and grisms. Larger grisms are carried on a dedicated slide for
spectroscopy. To eliminate sources of background noise, there are six
adjustable pupil masks available; four of them rotate with the telescope
pupil, and one is designed specifically for spectroscopy. The detector is a
32-channel, four-quadrant readout (1024x1024, Aladdin-3 InSb array). PHARO
(Hayward et al., 2001) is a near-infrared camera made by the Cornell
University Astronomy Department Infrared Group. It was made to work with the
200-inch Hale telescope at Palomar Observatory and the Palomar Adaptive Optics
system made by JPL. Detector has 1024 $\times$ 1024 Rockwell HAWAII HgCdTe
pixel array with wavelength sensitivity of 1 - 1.25 microns. It has
diffraction-limited angular resolutions of 0.063$\arcsec$ and 0.111$\arcsec$
for J and K band imaging, respectively. Its large-format detector has a field
of view of 25$\arcsec$ to 40$\arcsec$. The 3-m Shane telescope at Lick
Observatory uses the new ShaneAO adaptive optics technology in conjunction
with ShARCS (McGurk et al., 2014). ShARCS can perform low-dispersion grism
spectroscopy in the J, H, and K bands along with high-efficiency, diffraction-
limited imaging. With a HAWAII-2RG infrared detector, ShARCS can sample the
diffraction limit in all three wavelength bands with excellent quantum
efficiency (¿80%). To support future visible-light adaptive optics capacity,
the ShARCS device also has linear polarimetry capabilities and is sensitive
down to 650 nm. Each filter offers a FoV of 20$\arcsec$. NaCo is the Paranal
Observatory’s instrument, which is a combination of NAOS (Rousset et al.,
2000) (Nasmyth Adaptive Optics System) and CONICA (Lenzen et al., 1998) (Near-
Infrared Imager and Spectrograph) installed on the Very Large Telescope (VLT).
It is able to compensate for the atmospheric variabilities and provides a
diffraction-limited resolution for observing wavelengths ranging from 1 to 5
microns. It can collect imaging data with broad and narrow band filters, a
field of view of 14$\arcsec$-56$\arcsec$, and a pixel scale of 13-54 mas per
pixel.

##  4 Statistical Validation

With the advent of dedicated space missions for finding exoplanets, the number
of possible planet-like candidates has increased rapidly. This creates a
potential bottleneck between finding an exoplanet candidate and confirming the
discovery with multiple follow-up observations. It is expected that TESS alone
would be adding 12,000 potential exoplanets in the database over its 7-year
extended mission lifetime (Kunimoto et al., 2022). As a result, statistical
validation of exoplanets becomes a viable alternative to confirming each
candidate with dedicated observations with follow-up telescopes. Furthermore,
statistical validation of such likely candidates could also act as a vetting
and prioritization procedure for upcoming space missions and surveys such as
JWST or CHEOPS. The constant improvement in knowledge of exoplanets occurrence
rates and studies related to stellar populations have been utilised to derive
a statistical threshold for confidently validating transit events as
exoplanets.Various codes have been developed over the years with this
objective such as Pastis (Díaz et al., 2014), DAVE (Kostov et al., 2019),
VESPA and TRICERATOPS (Giacalone & Dressing, 2020). The last two have been
used in our work for this purpose.

We have chosen two different validation packages in order to mitigate any
potential biases being introduced due to the use of specific algorithms or
processes as has been suggested in previous studies Armstrong et al. (2021).
VESPA has been successfully deployed to validate $>1000$ exoplanets. Majority
of which were from the Kepler mission (Morton et al., 2016) and K2 mission
(Montet et al.; Christiansen et al.; Dressing et al.). It remains one of the
most widely used statistical validation frameworks for exoplanet validation
whereas TRICERATOPS was developed recently with a focus on the specifics of
the TESS mission profile adding to features of VESPA. It has shown positive
results for validations of TESS candidates (Giacalone et al., 2020). The
relative successful usage of these two frameworks combined with the ability to
negate bias was the driving factor behind choosing them.

###  4.1 Validation with VESPA

VESPA stands for Validation of Exoplanet Signals using a Probabilistic
Algorithm. It is an efficient automated tool to validate exoplanets using
TransitSignal and PopulationSet. Transit Signal composed of transit photometry
data, and PopulationSet includes PlanetPopulation, EBPopulation (Eclipsing
Binaries), HEBPopulation (Hierarchical Eclipsing Binaries) and BEBPopulation
(Blended/Background Eclipsing Binaries). VESPA uses TRILEGAL to simulate these
background star population. This set is then used to produce a prior
distribution for each astrophysical scenario using trapezoidal method. VESPA
calculates the false positive probability as follows:

$FPP=1-P_{pl}$ (1)

where,

$P_{pl}=\frac{\mathcal{L}_{pl}\pi_{pl}}{\mathcal{L}_{pl}\pi_{pl}+\mathcal{L}_{FP}\pi_{FP}}$
(2)

$\mathcal{L}_{i}$ represent model likelihood function, $\pi_{i}$ represent
model priors and $\mathcal{L}_{FP}\pi_{FP}$ is the sum of
$\mathcal{L}_{j}\pi_{j}$, where j stands for each false positive scenario.

We make use of VESPA version 0.6 through a virtual machine created by Kevin
Hardegree-Ullman 555https://github.com/kevinkhu/vespa-vm. The input parameters
required by VESPA in order to calculate FPP are located within three different
files: star.ini, fpp.ini, and transit.txt. The Effective Temperature, logg,
and Metallicity [Fe/H] are some of the stellar parameters that can be found in
the star.ini file. Other stellar parameters include the magnitude of the star
in various filters (B, V, J, H, K, etc.), as well as the magnitude that was
determined by the telescope. In this particular instance, we provided the TESS
magnitude of the target star. Included in the fpp.ini file are the following
parameters: orbital period, planet to star radius ratio, maximum aperture
radius (maxrad in arcsec), maximum permitted secondary depth of a potential
secondary eclipse (secthresh), position of target (RA and DEC), telescope
filter, and cadence (in days). We combined the Lightkurve (Lightkurve
Collaboration et al., 2018) and TLS (Hippke & Heller, 2019) packages in order
to determine these parameters based on TPF and Light Curve. We were able to
calculate maxrad by using an equation that was found in the VESPA
tutorial666https://github.com/timothydmorton/vespa-tutorial.git, by taking
into account a TESS plate-scale of 21 arcsec/pixel. The value of secthresh was
determined by $0.1\times(R_{P}$/$R_{S})^{2}$ (Christiansen et al., 2022b). We
retrieved additional required parameters from the ExoFOP-TESS website. The
transit photometry can be found in the file that goes by the name transit.txt.
It is required that the data be provided as a normalized, de-trended, and
phase-folded light curve. TLS and Lightkurve were used to process the light
curve in this manner. Along with these input files, we also provided a
contrast curve file generated using the high-resolution imaging (as discussed
in section 3). The contrast curve informs us of the relative brightness limit
of any nearby sources and can be used to rule out the presence of nearby stars
at specific radii brighter than a certain amount. We calculated FPP for each
selected target with 20 iterations and tabulated the mean and standard
deviation values in table 2.

###  4.2 Validation with TRICERATOPS

TRICERATOPS (Giacalone & Dressing, 2020) is used to validate planet candidates
using the Bayesian framework. The algorithm first starts searching for stars
within a 2.5’ radius of the target star. It determines the contamination of
the flux from these stars to the TESS aperture. For the target star and other
stars that seem to contribute enough to the transit signal, TRICERATOPS
calculates the probability of that signal being generated by a transiting
planet, an eclipsing binary, or a nearby eclipsing binary based on the
measurements of marginal likelihood for each scenario. This is then combined
with prior probability, based on which it calculates the final FPP and NFPP.
Mathematically it can be expressed as follows:

$\displaystyle FPP$ $\displaystyle=$ $\displaystyle
1-(\mathcal{P}_{TP}+\mathcal{P}_{PTP}+\mathcal{P}_{DTP})$ (3) $\displaystyle
NFPP$ $\displaystyle=$
$\displaystyle\Sigma(\mathcal{P}_{NTP}+\mathcal{P}_{NEB}+\mathcal{P}_{NEBX2P})$
(4)

Where $\mathcal{P}_{j}$ shows probability of each scenarios that can be found
on Table 1 of Giacalone et al. (2020), which can be calculated by,

$\displaystyle\mathcal{P}_{j}=\frac{p(S_{j}|D)}{\Sigma p(S_{j}|D)}$ (5)

where $p(S_{j}|D)\propto p(S_{j})p(D|S_{j})$. $p(S_{j})$ is prior probability
of each scenario and $p(D|S_{j})$ is Marginal likelihood or Bayesian Evidence.

Similar to VESPA, it can use high-resolution imaging follow-up observations to
constrain the area of sky around the target where an unresolved companion star
can exist. To calculate FPP and NFPP using TRICERATOPS we give following input
parameters and files: Orbital period in days, transit depth, data of transit
photometry, cadence in days, name of filter used by high resolution imaging
and data of contrast curve. We calculated FPP and NFPP for each selected
target with 15 iterations and tabulated the mean and standard deviation values
in table 2.

Table 2: False Positive Probabilities of all the targets calculated using VESPA and TRICERATOPS. $\mu$ represents the mean value and $\sigma$ represents the standard deviation in the values of FPP and NFPP. CC File depicts the name of the instrument (Filter Used) from which high resolution image was taken and respective filters used. VESPA is able to undertake multiple Contrast Curve (CC) files at one instance so only one FPP value is presented, while TRICERATOPS takes CC file one at a time so we calculated FPP and NFPP for each CC file separately. SNR = Signal to Noise Ratio and FAP = False Alarm Probability, calculated using TLS.  No. | TOI ID | TIC ID | SNR | FAP | VESPA | TRICERATOPS | CC File
---|---|---|---|---|---|---|---
|  |  |  | [%] |  $\mu$(FPP) $\pm$ $\sigma$(FPP) |  $\mu$(FPP) $\pm$ $\sigma$(FPP) |  $\mu$(NFPP) $\pm$ $\sigma$(NFPP) |
Validated Planets
1 | TOI 139 | TIC 62483237 |  |  |  |  |  |
|  | Sector 01 | 18.6619 | 0.01 | $1.75\times 10^{-04}\pm 4.08\times 10^{-05}$ | $7.88\times 10^{-04}\pm 4.88\times 10^{-04}$ | 0.00 $\pm$ 0.00 | ’Alopeke (562 nm)
|  | Sector 28 | 15.0097 | 0.01 | $3.48\times 10^{-03}\pm 5.70\times 10^{-04}$ | $9.03\times 10^{-04}\pm 2.87\times 10^{-04}$ | 0.00 $\pm$ 0.00
|  | Sector 01 |  |  |  | $2.25\times 10^{-04}\pm 7.13\times 10^{-05}$ | 0.00 $\pm$ 0.00 | ’Alopeke (832 nm)
|  | Sector 28 |  |  |  | $3.05\times 10^{-04}\pm 7.06\times 10^{-05}$ | 0.00 $\pm$ 0.00
|  | Sector 01 |  |  |  | $3.12\times 10^{-04}\pm 1.58\times 10^{-04}$ | 0.00 $\pm$ 0.00 | NIRC2 (BrGamma)
|  | Sector 28 |  |  |  | $3.34\times 10^{-04}\pm 2.16\times 10^{-04}$ | 0.00 $\pm$ 0.00
|  | Sector 01 |  |  |  | $3.78\times 10^{-04}\pm 1.99\times 10^{-04}$ | 0.00 $\pm$ 0.00 | NIRC2 (J)
|  | Sector 28 |  |  |  | $8.44\times 10^{-04}\pm 3.76\times 10^{-04}$ | 0.00 $\pm$ 0.00
2 | TOI 277 | 439456714 |  |  |  |  |  |
|  | Sector 03 | 19.1565 | 0.01 | $2.06\times 10^{-05}\pm 8.09\times 10^{-07}$ | $1.68\times 10^{-05}\pm 3.03\times 10^{-05}$ | 0.00 $\pm$ 0.00 | Zorro (562 nm)
|  | Sector 30 | 20.3263 | 0.01 | $3.93\times 10^{-03}\pm 1.01\times 10^{-03}$ | $5.86\times 10^{-06}\pm 8.90\times 10^{-06}$ | 0.00 $\pm$ 0.00
|  | Sector 03 |  |  |  | $3.21\times 10^{-05}\pm 5.97\times 10^{-05}$ | 0.00 $\pm$ 0.00 | Zorro (832 nm)
|  | Sector 30 |  |  |  | $4.83\times 10^{-06}\pm 3.90\times 10^{-06}$ | 0.00 $\pm$ 0.00
|  | Sector 03 |  |  |  | $5.49\times 10^{-05}\pm 8.29\times 10^{-05}$ | 0.00 $\pm$ 0.00 | ’Alopeke (562 nm)
|  | Sector 30 |  |  |  | $3.96\times 10^{-06}\pm 3.36\times 10^{-06}$ | 0.00 $\pm$ 0.00
|  | Sector 03 |  |  |  | $8.61\times 10^{-06}\pm 1.44\times 10^{-05}$ | 0.00 $\pm$ 0.00 | ’Alopeke (832 nm)
|  | Sector 30 |  |  |  | $6.66\times 10^{-06}\pm 9.65\times 10^{-06}$ | 0.00 $\pm$ 0.00
|  | Sector 03 |  |  |  | $5.06\times 10^{-04}\pm 5.45\times 10^{-04}$ | 0.00 $\pm$ 0.00 | NIRI (BrGamma)
|  | Sector 30 |  |  |  | $3.59\times 10^{-05}\pm 3.97\times 10^{-05}$ | 0.00 $\pm$ 0.00
3 | TOI 672 | 151825527 |  |  |  |  |  |
|  | Sector 09 | 43.1068 | 0.01 | 0.00 $\pm$ 0.00 | $7.34\times 10^{-09}\pm 9.90\times 10^{-09}$ | $2.52\times 10^{-13}\pm 2.63\times 10^{-13}$ | Zorro (562 nm)
|  | Sector 10 | 38.8176 | 0.01 | $1.52\times 10^{-08}\pm 8.66\times 10^{-06}$ | $5.56\times 10^{-07}\pm 2.00\times 10^{-06}$ | $5.14\times 10^{-13}\pm 2.56\times 10^{-13}$
|  | Sector 36 | 41.0399 | 0.01 | 0.00 $\pm$ 0.00 | $9.12\times 10^{-06}\pm 3.07\times 10^{-05}$ | $3.26\times 10^{-46}\pm 1.84\times 10^{-46}$
|  | Sector 09 |  |  |  | $2.01\times 10^{-07}\pm 4.45\times 10^{*07}$ | $1.20\times 10^{-13}\pm 6.99\times 10^{-14}$ | Zorro (832 nm)
|  | Sector 10 |  |  |  | $2.42\times 10^{-08}\pm 5.67\times 10^{*08}$ | $5.48\times 10^{-13}\pm 2.62\times 10^{-13}$
|  | Sector 36 |  |  |  | $6.76\times 10^{-08}\pm 1.99\times 10^{*07}$ | $2.71\times 10^{-46}\pm 1.68\times 10^{-46}$
4 | TOI 913 | 407126408 |  |  |  |  |  |
|  | Sector 12 | 15.6221 | 0.01 | $4.14\times 10^{-03}\pm 1.80\times 10^{-03}$ | $4.01\times 10^{-04}\pm 1.34\times 10^{-04}$ | $1.05\times 10^{-26}\pm 4.40\times 10^{-28}$ | Zorro (562 nm)
|  | Sector 13 | 16.5437 | 0.01 | $8.01\times 10^{-03}\pm 9.72\times 10^{-04}$ | $2.59\times 10^{-03}\pm 4.95\times 10^{-04}$ | $1.82\times 10^{-71}\pm 9.15\times 10^{-73}$
|  | Sector 12 |  |  |  | $1.04\times 10^{-04}\pm 3.71\times 10^{-05}$ | $1.11\times 10^{-26}\pm 5.58\times 10^{-28}$ | Zorro (832 nm)
|  | Sector 13 |  |  |  | $8.26\times 10^{-04}\pm 2.04\times 10^{-04}$ | $1.90\times 10^{-71}\pm 1.14\times 10^{-72}$
5 | TOI 1410 | 199444169 |  |  |  |  |  |
|  | Sector 16 | 22.9902 | 0.01 | $3.98\times 10^{-05}\pm 1.18\times 10^{-06}$ | $7.82\times 10^{-05}\pm 2.08\times 10^{-05}$ | $1.18\times 10^{-05}\pm 6.42\times 10^{-06}$ | PHARA (BrGamma)
|  | Sector 16 |  |  |  | $1.62\times 10^{-04}\pm 3.73\times 10^{-05}$ | $1.70\times 10^{-05}\pm 5.46\times 10^{-06}$ | ’Alopeke (562 nm)
|  | Sector 16 |  |  |  | $2.67\times 10^{-04}\pm 4.42\times 10^{-05}$ | $1.70\times 10^{-05}\pm 7.27\times 10^{-06}$ | ’Alopeke (832 nm)
|  | Sector 16 |  |  |  | $1.08\times 10^{-03}\pm 1.59\times 10^{-04}$ | $1.11\times 10^{-05}\pm 3.87\times 10^{-06}$ | NIRI (BrGamma)
6 | TOI 1694 | 396740648 |  |  |  |  |  |
|  | Sector 19 | 49.3381 | 0.01 | $1.49\times 10^{-05}\pm 3.61\times 10^{-07}$ | $1.76\times 10^{-03}\pm 2.53\times 10^{-03}$ | 0.00 $\pm$ 0.00 | ’Alopeke (562 nm)
|  | Sector 20 | 48.6979 | 0.01 | $3.91\times 10^{-07}\pm 1.36\times 10^{-05}$ | $1.59\times 10^{-03}\pm 2.52\times 10^{-03}$ | $5.26\times 10^{-108}\pm 6.93\times 10^{-108}$
|  | Sector 19 |  |  |  | $2.71\times 10^{-03}\pm 3.24\times 10^{-03}$ | 0.00 $\pm$ 0.00 | ’Alopeke (832 nm)
|  | Sector 20 |  |  |  | $2.82\times 10^{-03}\pm 3.74\times 10^{-03}$ | $6.73\times 10^{-108}\pm 1.14\times 10^{-107}$
|  | Sector 19 |  |  |  | $1.92\times 10^{-05}\pm 4.58\times 10^{-05}$ | 0.00 $\pm$ 0.00 | NIRC2 (Ks)
|  | Sector 20 |  |  |  | $8.93\times 10^{-06}\pm 1.69\times 10^{-05}$ | $3.51\times 10^{-108}\pm 5.77\times 10^{-108}$
7 | TOI 1801 | 119584412 |  |  |  |  |  |
|  | Sector 22 | 14.3160 | 0.01 | $3.04\times 10^{-04}\pm 5.39\times 10^{-06}$ | $1.92\times 10^{-06}\pm 2.10\times 10^{-06}$ | 0.00 $\pm$ 0.00 | ’Alopeke (562 nm)
|  | Sector 49 | 15.0856 | 0.01 | $2.44\times 10^{-03}\pm 4.68\times 10^{-04}$ | $5.10\times 10^{-06}\pm 1.24\times 10^{*06}$ | 0.00 $\pm$ 0.00
|  | Sector 22 |  |  |  | $1.63\times 10^{-06}\pm 1.28\times 10^{-06}$ | 0.00 $\pm$ 0.00 | ’Alopeke (832 nm)
|  | Sector 49 |  |  |  | $2.54\times 10^{-06}\pm 1.53\times 10^{-06}$ | 0.00 $\pm$ 0.00
|  | Sector 22 |  |  |  | $1.51\times 10^{-06}\pm 2.28\times 10^{-06}$ | 0.00 $\pm$ 0.00 | NIRC2 (BrGamma)
|  | Sector 49 |  |  |  | $2.03\times 10^{-06}\pm 1.17\times 10^{-06}$ | 0.00 $\pm$ 0.00
8 | TOI 1853 | 73540072 |  |  |  |  |  |
|  | Sector 50 | 13.0043 | 0.01 | $7.69\times 10^{-04}\pm 1.79\times 10^{-04}$ | $1.23\times 10^{-03}\pm 8.90\times 10^{-05}$ | 0.00 $\pm$ 0.00 | ’Alopeke (562 nm)
|  | Sector 50 |  |  |  | $1.50\times 10^{-03}\pm 1.38\times 10^{-04}$ | 0.00 $\pm$ 0.00 | ’Alopeke (832 nm)
|  | Sector 50 |  |  |  | $1.87\times 10^{-04}\pm 3.59\times 10^{-05}$ | 0.00 $\pm$ 0.00 | NIRC2 (BrGamma)
9 | TOI 2018 | 357501308 |  |  |  |  |  |
|  | Sector 24 | 23.8425 | 0.01 | 0.00 $\pm$ 0.00 | $3.09\times 10^{-06}\pm 3.21\times 10^{-06}$ | $2.29\times 10^{-18}\pm 3.17\times 10^{-19}$ | ’Alopeke (562 nm)
|  | Sector 51 | 15.7626 | 0.10 | 0.00 $\pm$ 0.00 | $3.88\times 10^{-07}\pm 2.07\times 10^{-07}$ | $1.34\times 10^{-7}\pm 9.08\times 10^{-09}$
|  | Sector 24 |  |  |  | $3.43\times 10^{-06}\pm 5.14\times 10^{-06}$ | $2.31\times 10^{-18}\pm 3.28\times 10^{-19}$ | ’Alopeke (832 nm)
|  | Sector 51 |  |  |  | $3.66\times 10^{-07}\pm 2.92\times 10^{-07}$ | $1.33\times 10^{-07}\pm 1.49\times 10^{-08}$
|  | Sector 24 |  |  |  | $1.42\times 10^{-05}\pm 1.33\times 10^{-05}$ | $2.03\times 10^{-18}\pm 2.48\times 10^{-19}$ | PHARO (BrGamma)
|  | Sector 51 |  |  |  | $8.67\times 10^{-07}\pm 9.27\times 10^{-07}$ | $1.22\times 10^{-07}\pm 1.29\times 10^{-08}$
|  | Sector 24 |  |  |  | $7.61\times 10^{-04}\pm 3.83\times 10^{-04}$ | $1.97\times 10^{-18}\pm 1.77\times 10^{-19}$ | ShARCS (BrGamma)
|  | Sector 51 |  |  |  | $1.09\times 10^{-04}\pm 3.98\times 10^{-05}$ | $1.14\times 10^{-17}\pm 8.23\times 10^{-19}$
|  | Sector 24 |  |  |  | $6.33\times 10^{-03}\pm 2.85\times 10^{-03}$ | $1.82\times 10^{-18}\pm 2.13\times 10^{-19}$ | ShARCS (J)
|  | Sector 51 |  |  |  | $8.87\times 10^{-04}\pm 1.88\times 10^{-04}$ | $1.17\times 10^{-07}\pm 1.27\times 10^{-08}$
10 | TOI 2134 | 75878355 |  |  |  |  |  |
|  | Sector 26 | 50.6457 | 0.01 | $9.63\times 10^{-05}\pm 3.68\times 10^{-06}$ | $1.09\times 10^{-14}\pm 3.04\times 10^{-14}$ | $7.76\times 10^{-63}\pm 7.02\times 10^{-63}$ | PHARO (BrGamma)
|  | Sector 40 | 50.9617 | 0.01 | $9.72\times 10^{-08}\pm 2.72\times 10^{-09}$ | $4.49\times 10^{-08}\pm 1.62\times 10^{-07}$ | $4.75\times 10^{-39}\pm 2.63\times 10^{-39}$
|  | Sector 52 | 28.9029 | 0.01 | $1.82\times 10^{-07}\pm 4.73\times 10^{-09}$ | $1.67\times 10^{-12}\pm 6.26\times 10^{-12}$ | $1.35\times 10^{-37}\pm 2.22\times 10^{-38}$
|  | Sector 53 | 48.3616 | 0.01 | $7.41\times 10^{-07}\pm 1.87\times 10^{-08}$ | $3.09\times 10^{-11}\pm 1.41\times 10^{-11}$ | $2.32\times 10^{-49}\pm 1.37\times 10^{-49}$
|  | Sector 54 | 46.0235 | 0.01 | $6.54\times 10^{-03}\pm 8.68\times 10^{-04}$ | $8.87\times 10^{-14}\pm 3.22\times 10^{-13}$ | $5.45\times 10^{-58}\pm 3.21\times 10^{-58}$
11 | TOI 2194 | 271478281 |  |  |  |  |  |
|  | Sector 27 | 29.3712 | 0.01 | $1.46\times 10^{-06}\pm 1.41\times 10^{-06}$ | $1.32\times 10^{-06}\pm 3.88\times 10^{-06}$ | 0.00 $\pm$ 0.00 | HRCam (I)
12 | TOI 2443 | 318753380 |  |  |  |  |  |
|  | Sector 31 | 33.3454 | 0.01 | 0.00 $\pm$ 0.00 | $1.58\times 10^{-17}\pm 8.24\times 10^{-17}$ | $1.97\times 10^{-19}\pm 1.00\times 10^{-19}$ | ’Alopeke (562 nm)
|  | Sector 31 |  |  |  | $1.05\times 10^{-13}\pm 3.95\times 10^{-13}$ | $2.28\times 10^{-19}\pm 1.21\times 10^{-19}$ | ’Alopeke (832 nm)
|  | Sector 31 |  |  |  | $1.11\times 10^{-11}\pm 3.55\times 10^{-11}$ | $1.50\times 10^{-19}\pm 5.81\times 10^{-20}$ | PHARO (BrGamma)
13 | TOI 2459 | 192790476 |  |  |  |  |  |
|  | Sector 05 |  |  | $8.66\times 10^{-03}\pm 1.05\times 10^{-03}$ | $8.52\times 10^{-04}\pm 7.63\times 10^{-05}$ | $8.28\times 10^{-04}\pm 6.07\times 10^{-05}$ | HRCam (I)
|  | Sector 06 |  |  | $1.49\times 10^{-05}\pm 3.61\times 10^{-07}$ | $3.71\times 10^{-04}\pm 2.03\times 10^{-04}$ | $2.56\times 10^{-04}\pm 2.04\times 10^{-05}$
|  | Sector 32 |  |  | $4.28\times 10^{-03}\pm 1.62\times 10^{-04}$ | $2.44\times 10^{-06}\pm 6.22\times 10^{-06}$ | $1.44\times 10^{-07}\pm 1.67\times 10^{-08}$
|  | Sector 33 |  |  | $1.54\times 10^{-04}\pm 3.51\times 10^{-06}$ | $7.08\times 10^{-04}\pm 6.01\times 10^{-05}$ | $6.98\times 10^{-04}\pm 4.91\times 10^{-05}$
14 | TOI 3082 | 428699140 |  |  |  |  |  |
|  | Sector 37 | 16.8096 | 0.01 | $4.08\times 10^{-04}\pm 2.02\times 10^{-04}$ | $6.78\times 10^{-03}\pm 1.06\times 10^{-03}$ | $1.39\times 10^{-27}\pm 1.06\times 10^{-27}$ | -
15 | TOI 4308 | 144193715 |  |  |  |  |  |
|  | Sector 01 | 8.9739 | 0.01 | $3.54\times 10^{-03}\pm 3.49\times 10^{-04}$ | $5.98\times 10^{-03}\pm 3.63\times 10^{-04}$ | $1.64\times 10^{-10}\pm 2.40\times 10^{-11}$ | HRCam (I)
16 | TOI 5803 | 466382581 |  |  |  |  |  |
|  | Sector 55 | 18.9821 | 0.01 | $1.22\times 10^{-03}\pm 4.05\times 10^{-04}$ | $9.31\times 10^{-03}\pm 2.74\times 10^{-03}$ | $4.54\times 10^{-08}\pm 3.21\times 10^{-09}$ | HRCam (I)
17 | TOI 1732 | 470987100 |  |  |  |  |  |
|  | Sector 20 | 10.6478 | 0.01 | $2.51\times 10^{-02}\pm 2.74\times 10^{-03}$ | $8.10\times 10^{-03}\pm 1.26\times 10^{-04}$ | $7.33\times 10^{-03}\pm 1.37\times 10^{-04}$ | PHARO (BrGamma)
|  | Sector 47 | 12.6158 | 0.01 | $6.01\times 10^{-03}\pm 1.12\times 10^{-03}$ | $2.45\times 10^{-04}\pm 9.89\times 10^{-06}$ | $2.15\times 10^{-04}\pm 6.56\times 10^{-06}$
|  | Sector 20 |  |  |  | $1.02\times 10^{-02}\pm 1.53\times 10^{-04}$ | $8.08\times 10^{-03}\pm 1.46\times 10^{-04}$ | ’Alopeke (562 nm)
|  | Sector 47 |  |  |  | $2.72\times 10^{-04}\pm 1.46\times 10^{-05}$ | $3.37\times 10^{-04}\pm 1.34\times 10^{-05}$
|  | Sector 20 |  |  |  | $8.84\times 10^{-03}\pm 2.44\times 10^{-04}$ | $8.26\times 10^{-03}\pm 2.43\times 10^{-04}$ | ’Alopeke (832 nm)
|  | Sector 47 |  |  |  | $2.45\times 10^{-04}\pm 1.01\times 10^{-05}$ | $2.34\times 10^{-04}\pm 7.39\times 10^{-06}$
|  | Sector 20 |  |  |  | $1.17\times 10^{-02}\pm 1.64\times 10^{-04}$ | $6.97\times 10^{-03}\pm 9.31\times 10^{-05}$ | ShARCS (K)
|  | Sector 47 |  |  |  | $3.92\times 10^{-04}\pm 2.86\times 10^{-05}$ | $2.07\times 10^{-04}\pm 1.06\times 10^{-05}$
18 | TOI 2200 | 142105158 |  |  |  |  |  |
|  | Sector 27 | 31.8576 | 0.01 | $6.32\times 10^{-05}\pm 9.34\times 10^{-06}$ | $1.05\times 10^{-01}\pm 5.56\times 10^{-02}$ | $1.15\times 10^{-19}\pm 3.67\times 10^{-10}$ | -
|  | Sector 28 | 33.0523 | 0.01 | $1.81\times 10^{-04}\pm 1.70\times 10^{-04}$ | $1.46\times 10^{-01}\pm 5.07\times 10^{-02}$ | $2.01\times 10^{-07}\pm 5.37\times 10^{-08}$
|  | Sector 29 | 35.2422 | 0.01 | $8.44\times 10^{-05}\pm 1.36\times 10^{-05}$ | $6.15\times 10^{-02}\pm 2.88\times 10^{-02}$ | $7.44\times 10^{-12}\pm 2.17\times 10^{-12}$
|  | Sector 30 | 34.8712 | 0.01 | $6.18\times 10^{-03}\pm 4.71\times 10^{-03}$ | $5.01\times 10^{-01}\pm 9.29\times 10^{-02}$ | $2.95\times 10^{-06}\pm 4.58\times 10^{-08}$
|  | Sector 31 | 33.0510 | 0.01 | $2.64\times 10^{-04}\pm 5.39\times 10^{-05}$ | $5.85\times 10^{-02}\pm 2.04\times 10^{-02}$ | $1.48\times 10^{-10}\pm 4.34\times 10^{-11}$
|  | Sector 32 | 33.4764 | 0.01 | $2.40\times 10^{-04}\pm 9.77\times 10^{-06}$ | $3.94\times 10^{-02}\pm 2.08\times 10^{-02}$ | $2.83\times 10^{-14}\pm 1.28\times 10^{-14}$
|  | Sector 33 | 34.5528 | 0.01 | $1.55\times 10^{-03}\pm 7.53\times 10^{-04}$ | $4.82\times 10^{-01}\pm 9.15\times 10^{-02}$ | $2.42\times 10^{-05}\pm 4.74\times 10^{-06}$
|  | Sector 34 | 35.6292 | 0.01 | $2.11\times 10^{-05}\pm 7.26\times 10^{-07}$ | $2.95\times 10^{-01}\pm 6.65\times 10^{-02}$ | $5.68\times 10^{-10}\pm 2.01\times 10^{-10}$
|  | Sector 36 | 33.9929 | 0.01 | $1.47\times 10^{-03}\pm 5.87\times 10^{-04}$ | $3.52\times 10^{-01}\pm 9.12\times 10^{-02}$ | $6.92\times 10^{-05}\pm 9.69\times 10^{-05}$
|  | Sector 37 | 34.8538 | 0.01 | $3.75\times 10^{-04}\pm 1.38\times 10^{-05}$ | $7.23\times 10^{-02}\pm 2.41\times 10^{-02}$ | $5.37\times 10^{-13}\pm 1.13\times 10^{-13}$
|  | Sector 38 | 34.9817 | 0.01 | $1.22\times 10^{-03}\pm 6.33\times 10^{-04}$ | $1.13\times 10^{-01}\pm 4.40\times 10^{-02}$ | $1.19\times 10^{-10}\pm 3.36\times 10^{-11}$
|  | Sector 39 | 37.0436 | 0.01 | $9.25\times 10^{-03}\pm 9.94\times 10^{-03}$ | $4.86\times 10^{-01}\pm 1.21\times 10^{-01}$ | $1.01\times 10^{-08}\pm 3.36\times 10^{-09}$
19 | TOI 5704 | 148673433 |  |  |  |  |  |
|  | Sector 22 | 18.0160 | 0.01 | $2.16\times 10^{-02}\pm 3.59\times 10^{-03}$ | $8.56\times 10^{-03}\pm 4.97\times 10^{-05}$ | $5.51\times 10^{-04}\pm 1.49\times 10^{-05}$ | -
|  | Sector 48 | 16.8362 | 0.01 | $1.57\times 10^{-02}\pm 7.75\times 10^{-03}$ | $6.61\times 10^{-03}\pm 1.03\times 10^{-03}$ | $5.82\times 10^{-06}\pm 5.28\times 10^{-07}$
20 | TOI 323 | 251852984 |  |  |  |  |  |
|  | Sector 37 | 12.8622 | 0.01 | $1.10\times 10^{-02}\pm 1.46\times 10^{-03}$ | $2.49\times 10^{-01}\pm 2.30\times 10^{-02}$ | $3.20\times 10^{-11}\pm 7.36\times 10^{-12}$ | ’Alopeke (562 nm)
|  | Sector 37 |  |  |  | $2.57\times 10^{-01}\pm 2.75\times 10^{-02}$ | $3.59\times 10^{-11}\pm 5.88\times 10^{-12}$ | ’Alopeke (832 nm)
|  | Sector 37 |  |  |  | $2.56\times 10^{-01}\pm 2.09\times 10^{-02}$ | $2.78\times 10^{-11}\pm 4.54\times 10^{-12}$ | NaCo (K)
21 | TOI 815 | 102840239 |  |  |  |  |  |
|  | Sector 36 | 15.7674 | 1.00 | $7.13\times 10^{*03}\pm 2.71\times 10^{-03}$ | $2.23\times 10^{-03}\pm 1.32\times 10^{-03}$ | $1.87\times 10^{-03}\pm 1.32\times 10^{-03}$ | Zorro (562 nm)
|  | Sector 36 |  |  |  | $2.13\times 10^{-03}\pm 1.32\times 10^{-03}$ | $1.77\times 10^{-03}\pm 1.32\times 10^{-03}$ | Zorro (832 nm)
22 | TOI 493 | 19025965 |  |  |  |  |  |
|  | Sector 34 | 9.4971 | 0.01 | $8.75\times 10^{-02}\pm 5.47\times 10^{-03}$ | $1.75\times 10^{-02}\pm 1.62\times 10^{-03}$ | $3.31\times 10^{-03}\pm 5.99\times 10^{-04}$ | NIRI (BrGamma)
|  | Sector 44 | 14.7922 | 0.01 | $3.05\times 10^{-03}\pm 6.33\times 10^{-04}$ | $1.41\times 10^{-02}\pm 3.09\times 10^{-03}$ | $1.06\times 10^{-02}\pm 2.51\times 10^{-03}$
|  | Sector 45 | 12.3651 | 0.01 | $2.53\times 10^{-04}\pm 6.27\times 10^{-06}$ | $2.24\times 10^{-02}\pm 3.61\times 10^{-03}$ | $1.88\times 10^{-02}\pm 3.45\times 10^{-03}$
|  | Sector 46 | 9.7146 | 0.01 | $5.27\times 10^{-03}\pm 1.09\times 10^{-03}$ | $2.83\times 10^{-02}\pm 7.96\times 10^{-03}$ | $1.72\times 10^{-02}\pm 7.69\times 10^{-03}$
|  | Sector 34 |  |  |  | $1.23\times 10^{-02}\pm 1.62\times 10^{-03}$ | $3.56\times 10^{-03}\pm 6.47\times 10^{-04}$ | NIRC2 (BrGamma)
|  | Sector 44 |  |  |  | $1.08\times 10^{-02}\pm 2.07\times 10^{-03}$ | $1.00\times 10^{-02}\pm 1.85\times 10^{-03}$
|  | Sector 45 |  |  |  | $1.94\times 10^{-02}\pm 4.41\times 10^{-03}$ | $1.87\times 10^{-02}\pm 4.39\times 10^{-03}$
|  | Sector 46 |  |  |  | $2.99\times 10^{-02}\pm 9.54\times 10^{-03}$ | $2.28\times 10^{-02}\pm 9.19\times 10^{-03}$
23 | TOI 1179 | 148914726 |  |  |  |  |  |
|  | Sector 14 | 41.5323 | 0.01 | $8.70\times 10^{-05}\pm 2.36\times 10^{-05}$ | $9.98\times 10^{-01}\pm 1.51\times 10^{-03}$ | $2.79\times 10^{-02}\pm 9.85\times 10^{-03}$ | ’Alopeke (562 nm)
|  | Sector 15 | 47.9257 | 0.01 | $3.87\times 10^{-05}\pm 1.15\times 10^{-05}$ | $9.87\times 10^{-01}\pm 6.69\times 10^{-03}$ | $7.11\times 10^{-02}\pm 2.72\times 10^{-02}$
|  | Sector 21 | 49.6108 | 0.01 | $5.89\times 10^{-06}\pm 4.26\times 10^{-06}$ | $9.72\times 10^{-01}\pm 1.57\times 10^{-02}$ | $5.84\times 10^{-02}\pm 2.29\times 10^{-02}$
|  | Sector 22 | 43.6678 | 0.01 | $5.97\times 10^{-07}\pm 2.16\times 10^{-07}$ | $2.51\times 10^{-02}\pm 5.48\times 10^{-03}$ | $4.08\times 10^{-03}\pm 1.48\times 10^{-03}$
|  | Sector 41 | 42.6402 | 0.01 | Error | $1.56\times 10^{-01}\pm 7.08\times 10^{-02}$ | $3.46\times 10^{-02}\pm 2.20\times 10^{-02}$
|  | Sector 48 | 42.5446 | 0.01 | $2.24\times 10^{-04}\pm 4.54\times 10^{-05}$ | $9.82\times 10^{-01}\pm 7.00\times 10^{-03}$ | $1.20\times 10^{-01}\pm 4.19\times 10^{-02}$
|  | Sector 14 |  |  |  | $9.96\times 10^{-01}\pm 4.87\times 10^{-03}$ | $2.78\times 10^{*01}\pm 7.95\times 10^{-03}$ | ’Alopeke (832 nm)
|  | Sector 15 |  |  |  | $9.78\times 10^{-01}\pm 1.98\times 10^{-02}$ | $9.48\times 10^{-02}\pm 2.78\times 10^{-02}$
|  | Sector 21 |  |  |  | $9.82\times 10^{-01}\pm 1.02\times 10^{-02}$ | $7.31\times 10^{-02}\pm 2.08\times 10^{-02}$
|  | Sector 22 |  |  |  | $2.17\times 10^{-02}\pm 6.25\times 10^{-03}$ | $4.69\times 10^{-03}\pm 1.74\times 10^{-03}$
|  | Sector 41 |  |  |  | $1.32\times 10^{-01}\pm 9.88\times 10^{-02}$ | $4.59\times 10^{-02}\pm 3.57\times 10^{-02}$
|  | Sector 48 |  |  |  | $9.67\times 10^{-01}\pm 2.17\times 10^{-02}$ | $1.67\times 10^{-01}\pm 4.12\times 10^{-02}$
24 | TOI 1180 | 158002130 |  |  |  |  |  |
|  | Sector 14 | 17.9456 | 0.01 | $2.09\times 10^{-02}\pm 6.46\times 10^{-03}$ | $7.99\times 10^{-03}\pm 5.87\times 10^{-04}$ | $7.13\times 10^{-04}\pm 2.59\times 10^{-05}$ | Speckle Polarimeter (I)
|  | Sector 19 | 19.8802 | 0.01 | $1.02\times 10^{-02}\pm 3.52\times 10^{-03}$ | $6.56\times 10^{-03}\pm 1.13\times 10^{-03}$ | $2.34\times 10^{-04}\pm 1.67\times 10^{-05}$
|  | Sector 20 | 13.5258 | 0.01 | Error | $1.28\times 10^{-02}\pm 1.48\times 10^{-03}$ | $4.39\times 10^{-03}\pm 1.13\times 10^{-04}$
|  | Sector 21 | 13.9659 | 0.01 | $9.13\times 10^{-02}\pm 1.35\times 10^{-02}$ | $1.30\times 10^{-02}\pm 1.14\times 10^{-03}$ | $4.31\times 10^{-03}\pm 1.15\times 10^{-04}$
|  | Sector 40 | 20.0742 | 0.01 | $1.36\times 10^{-03}\pm 1.74\times 10^{-03}$ | $5.07\times 10^{-03}\pm 1.15\times 10^{-03}$ | $1.71\times 10^{-05}\pm 2.48\times 10^{-06}$
|  | Sector 41 | 11.1516 | 0.01 | $1.98\times 10^{-04}\pm 4.89\times 10^{-06}$ | $4.87\times 10^{-03}\pm 1.11\times 10^{-03}$ | $2.22\times 10^{-05}\pm 3.03\times 10^{-06}$
|  | Sector 47 | 17.2377 | 0.01 | $1.54\times 10^{-01}\pm 3.68\times 10^{-02}$ | $1.86\times 10^{-02}\pm 2.32\times 10^{-03}$ | $9.15\times 10^{-03}\pm 8.68\times 10^{-04}$
|  | Sector 48 | 17.6670 | 0.01 | $9.02\times 10^{-02}\pm 3.51\times 10^{-02}$ | $3.99\times 10^{-02}\pm 3.78\times 10^{-03}$ | $1.86\times 10^{-02}\pm 1.40\times 10^{-03}$
25 | TOI 2408 | 67630845 |  |  |  |  |  |
|  | Sector 30 | 19.5685 | 0.01 | $3.52\times 10^{-01}\pm 2.68\times 10^{-01}$ | $1.75\times 10^{-01}\pm 2.89\times 10^{-02}$ | 0.00 $\pm$ 0.00 | -
26 | TOI 3568 | 160390955 |  |  |  |  |  |
|  | Sector 55 | 21.0566 | 0.01 | $4.30\times 10^{-05}\pm 2.08\times 10^{-06}$ | $1.17\times 10^{-02}\pm 6.66\times 10^{-03}$ | $1.88\times 10^{-03}\pm 3.82\times 10^{-04}$ | NIRC2 (K)
|  | Sector 55 |  |  |  | $3.61\times 10^{-02}\pm 1.07\times 10^{-02}$ | $2.22\times 10^{-03}\pm 4.26\times 10^{-04}$ | PHARO (Hcont)
|  | Sector 55 |  |  |  | $2.32\times 10^{-03}\pm 3.36\times 10^{-03}$ | $2.09\times 10^{-03}\pm 5.63\times 10^{-04}$ | PHARO (BrGamma)
27 | TOI 3896 | 445837596 |  |  |  |  |  |
|  | Sector 48 | 11.1953 | 0.01 | Error | $1.40\times 10^{-02}\pm 8.42\times 10^{-04}$ | $1.04\times 10^{-03}\pm 3.75\times 10^{-05}$ | PHARO (BrGamma)
28 | TOI 3913 | 155898758 |  |  |  |  |  |
|  | Sector 49 | 16.1696 | 0.01 | $1.34\times 10^{-02}\pm 1.80\times 10^{-03}$ | $6.16\times 10^{-01}\pm 4.30\times 10^{-02}$ | 0.00 $\pm$ 0.00 | PHARO (BrGamma)
|  | Sector 50 | 14.5601 | 0.01 | $8.86\times 10^{-03}\pm 8.02\times 10^{-04}$ | $5.63\times 10^{-02}\pm 6.18\times 10^{-03}$ | 0.00 $\pm$ 0.00
29 | TOI 4090 | 289373041 |  |  |  |  |  |
|  | Sector 53 | 12.7536 | 0.01 | $5.07\times 10^{-02}\pm 3.78\times 10^{-03}$ | $3.95\times 10^{-02}\pm 4.76\times 10^{-03}$ | $2.51\times 10^{-02}\pm 1.69\times 10^{-03}$ | PHARO (BrGamma)
|  | Sector 54 | 15.2323 | 0.01 | $1.23\times 10^{-02}\pm 4.69\times 10^{-03}$ | $5.63\times 10^{-02}\pm 6.18\times 10^{-03}$ | $2.82\times 10^{-02}\pm 2.79\times 10^{-03}$
30 | TOI 5584 | 29169215 |  |  |  |  |  |
|  | Sector 21 | 13.8631 | 0.01 | $3.73\times 10^{-01}\pm 2.72\times 10^{-02}$ | $1.91\times 10^{-02}\pm 1.33\times 10^{-03}$ | $7.18\times 10^{-03}\pm 4.19\times 10^{-04}$ | -
|  | Sector 47 | 7.0555 | 0.10 | $8.76\times 10^{-01}\pm 1.52\times 10^{-02}$ | $1.81\times 10^{-01}\pm 6.31\times 10^{-03}$ | $1.46\times 10^{-01}\pm 5.59\times 10^{-03}$

##  5 Validated Planets

We consider planetary candidates with high-resolution imaging showing no
evidence of stellar companion, VESPA FPP of $<1\%$ (Morton, 2012) and
TRICERATOPS FPP of $<1.5\times 10^{-2}$ and NFPP of $<10^{-3}$ (Giacalone &
Dressing, 2020) to be statistically validated. By examining the 30 candidates
we validated 16 planetary systems. The properties of the new planets are shown
in the top panel and the properties of new host stars are shown in the bottom
panel of Figure 1. From total of 16 newly validated planets, TOI-1410b and
TOI-1853b are short period planets with orbital period 1.22 and 1.24 days
respectively, and in size from the super-Earth sized TOI-2194b (1.99
$R_{\earth}$) and TOI-1801b (2.09 $R_{\earth}$) to the sub-Saturn sized
TOI-672b (5.26 $R_{\earth}$) and TOI-1694b (5.46 $R_{\earth}$). Derived
planetary and orbital parameters are listed in Table 4. Phase-folded transit
light curves with the best-fit Juliet model are shown in Figure 2 and Figure
3.

Figure 1: Properties of newly validated systems. Top panel: New planets and
their comparison with previously known planets (with $<$ 100-day period),
shaded region depicts the Hot Neptune Desert, figure in right panel is a
zoomed-in version of the left figure with labels for the planets in the Hot
Neptune Desert. Seven of the planets lie in the Hot-Neptune Desert. Right
panel: New host stars compared to hosts of known planets. Data for this plots
were taken from NASA Exoplanet Archive.

In this section we will discuss some of the interesting features of new
systems. By using an unbiased mass-radius empirical relationship (Chen &
Kipping, 2017), which was developed upon the probabilistic mass-radius
relation condition on a sample we approximated the mass of the newly validated
planets. It is to be noted here that these mass estimates should not be
considered robust for characterization of the planets properties, we used
these estimates to get better idea of these systems. Based on this mass
estimates we also calculated the semi-amplitude of radial velocity, that is
induced on the host star by the orbiting planet. In order to facilitate the
identification of the most optimal targets for atmospheric characterization
among the TESS planet candidates, Kempton et al. (2018) developed a method for
calculating Transmission Spectroscopy Metrics (TSM) and Emission Spectroscopy
Metrics (ESM) by taking into account various parameters such as the brightness
of the host star, planetary radius, mass and equilibrium temperature. These
metrics provide a simple method for estimating the expected signal-to-noise
ratio of the James Webb Space Telescope (JWST) in both transmission and
thermal emission spectroscopy for a given planet. The calculated TSM and ESM
values for the candidates are tabulated in Table 3. This method allows for
efficient prioritization of the most promising candidates for further study
and characterization of their atmospheric properties. Distribution of TSM and
ESM for planets is shown in Figure 4. Using radial velocity mass measurements,
it is recommended to quickly measure the original mass and follow up on
targets that meet the suggested threshold values for these measurements.

Table 3: Estimated parameters, Transmission and Emission Spectroscopy Metrics (TSM and ESM) for newly validated planetary systems. Planet | TIC ID | $T_{eq}$ | $M_{p}$ | Density | K | TSM | ESM
---|---|---|---|---|---|---|---
|  | [K] | [$M_{\earth}$] | [cgs] | m $s^{-1}$ |  |
TOI-139b | 62483237 | 561.17 | 6.6179 | 2.45 | 2.4305 | 68.30 | 3.18
TOI-277b | 439456714 | 739.90 | 9.8010 | 1.82 | 6.1001 | 86.95 | 10.34
TOI-672b | 151825527 | 676.15 | 24.1481 | 0.91 | 15.1375 | 134.15 | 22.93
TOI-913b | 407126408 | 712.01 | 6.6003 | 2.46 | 2.1586 | 63.70 | 3.96
TOI-1410b | 199444169 | 1181.44 | 10.6133 | 1.71 | 7.3854 | 113.18 | 18.04
TOI-1694b | 396740648 | 1136.57 | 25.7142 | 0.87 | 11.8096 | 125.91 | 25.89
TOI-1801b | 119584412 | 490.47 | 5.0231 | 3.03 | 2.1975 | 70.17 | 2.77
TOI-1853b | 73540072 | 1510.96 | 12.8946 | 1.47 | 8.7308 | 78.28 | 13.57
TOI-2018b | 357501308 | 652.44 | 5.8638 | 2.69 | 2.5327 | 116.93 | 7.55
TOI-2134b | 75878355 | 665.25 | 9.0899 | 1.92 | 3.5471 | 181.15 | 13.12
TOI-2194b | 271478281 | 590.88 | 4.6230 | 3.23 | 1.4536 | 131.02 | 5.45
TOI-2443b | 318753380 | 600.83 | 8.1321 | 2.09 | 2.7401 | 132.89 | 8.28
TOI-2459b | 192790476 | 445.01 | 9.0497 | 1.93 | 2.8544 | 76.04 | 2.46
TOI-3082b | 428699140 | 1032.78 | 13.0463 | 1.46 | 8.7974 | 78.37 | 13.96
TOI-4308b | 144193715 | 763.05 | 6.4460 | 2.50 | 2.1129 | 39.68 | 2.47
TOI-5803b | 466382581 | 678.87 | 10.7798 | 1.69 | 4.3137 | 69.69 | 4.55
Table 4: Planetary and orbital parameters for the newly validated planetary systems using Juliet.  Planet | TIC ID | Period | Epoch Time | $R_{p}/R_{s}$ | $R_{p}$ | b | $a/R_{s}$ | i
---|---|---|---|---|---|---|---|---
|  | [days] | [BJD] |  | [$R_{\earth}$] |  |  | [degree]
TOI-139b | 62483237 | $11.070850^{+0.000024}_{-0.000030}$ | $2458334.8906^{+0.0010}_{-0.0010}$ | $0.0321^{+0.0028}_{-0.0016}$ | $2.4566^{+0.2122}_{-0.1245}$ | $0.395^{+0.254}_{-0.252}$ | $33.159^{+2.667}_{-5.336}$ | $89.32^{+0.45}_{-0.65}$
TOI-277b | 439456714 | $3.994086^{+0.000008}_{-0.000009}$ | $2458385.0362^{+0.0008}_{-0.0008}$ | $0.0541^{+0.0052}_{-0.0026}$ | $3.0950^{+0.2958}_{-0.1475}$ | $0.402^{+0.300}_{-0.253}$ | $13.650^{+1.114}_{-2.828}$ | $88.32^{+1.10}_{-2.00}$
TOI-672b | 151825527 | $3.633575^{+0.000001}_{-0.000001}$ | $2458546.4799^{+0.0002}_{-0.0002}$ | $0.0885^{+0.0014}_{-0.0017}$ | $5.2604^{+0.0827}_{-0.0985}$ | $0.424^{+0.108}_{-0.206}$ | $15.503^{+1.055}_{-0.934}$ | $88.43^{+0.82}_{-0.52}$
TOI-913b | 407126408 | $11.098644^{+0.000587}_{-0.000581}$ | $2458625.2133^{+0.0024}_{-0.0023}$ | $0.0306^{+0.0016}_{-0.0013}$ | $2.4528^{+0.1269}_{-0.1009}$ | $0.387^{+0.248}_{-0.254}$ | $24.352^{+1.910}_{-3.825}$ | $89.10^{+0.61}_{-0.87}$
TOI-1410b | 199444169 | $1.216901^{+0.000038}_{-0.000038}$ | $2458739.7294^{+0.0004}_{-0.0004}$ | $0.0381^{+0.0018}_{-0.0014}$ | $3.2434^{+0.1541}_{-0.1167}$ | $0.456^{+0.247}_{-0.273}$ | $7.806^{+0.822}_{-1.560}$ | $86.64^{+2.13}_{-3.11}$
TOI-1694b | 396740648 | $3.770179^{+0.000058}_{-0.000060}$ | $2458817.2662^{+0.0004}_{-0.0007}$ | $0.0610^{+0.0017}_{-0.0013}$ | $5.4585^{+0.4682}_{-0.7919}$ | $0.326^{+0.172}_{-0.198}$ | $10.206^{+0.468}_{-0.792}$ | $88.17^{+1.15}_{-1.19}$
TOI-1801b | 119584412 | $10.643976^{+0.000014}_{-0.000014}$ | $2458903.5427^{+0.0008}_{-0.0008}$ | $0.0350^{+0.0010}_{-0.0011}$ | $2.0888^{+0.0606}_{-0.0655}$ | $0.266^{+0.179}_{-0.180}$ | $30.251^{+1.152}_{-2.157}$ | $89.50^{+0.34}_{-0.40}$
TOI-1853b | 73540072 | $1.243702^{+0.000121}_{-0.000114}$ | $2459690.7422^{+0.0012}_{-0.0012}$ | $0.0396^{+0.0024}_{-0.0020}$ | $3.6369^{+0.2200}_{-0.1845}$ | $0.371^{+0.276}_{-0.247}$ | $5.865^{+0.500}_{-0.974}$ | $86.37^{+2.52}_{-3.92}$
TOI-2018b | 357501308 | $7.435588^{+0.000009}_{-0.000009}$ | $2458958.2582^{+0.0006}_{-0.0007}$ | $0.0336^{+0.0014}_{-0.0011}$ | $2.2879^{+0.0929}_{-0.0742}$ | $0.475^{+0.211}_{-0.274}$ | $22.206^{+2.503}_{-3.775}$ | $88.78^{+0.75}_{-0.91}$
TOI-2134b | 75878355 | $9.229197^{+0.000003}_{-0.000004}$ | $2459010.6896^{+0.0002}_{-0.0002}$ | $0.0352^{+0.0008}_{-0.0005}$ | $2.9608^{+0.0697}_{-0.0394}$ | $0.301^{+0.172}_{-0.185}$ | $23.585^{+0.926}_{-1.755}$ | $89.27^{+0.46}_{-0.55}$
TOI-2194b | 271478281 | $15.337597^{+0.001585}_{-0.001616}$ | $2459037.3678^{+0.0013}_{-0.0011}$ | $0.0263^{+0.0017}_{-0.0009}$ | $1.9892^{+0.1313}_{-0.0668}$ | $0.412^{+0.288}_{-0.253}$ | $32.393^{+2.718}_{-6.864}$ | $89.27^{+0.47}_{-0.85}$
TOI-2443b | 318753380 | $15.669494^{+0.000926}_{-0.001004}$ | $2459148.0988^{+0.0007}_{-0.0007}$ | $0.0347^{+0.0006}_{-0.0006}$ | $2.7731^{+0.0493}_{-0.0515}$ | $0.285^{+0.183}_{-0.175}$ | $26.293^{+0.952}_{-2.053}$ | $89.38^{+0.39}_{-0.48}$
TOI-2459b | 192790476 | $19.104718^{+0.000023}_{-0.000024}$ | $2458452.3342^{+0.0007}_{-0.0007}$ | $0.0400^{+0.0012}_{-0.0009}$ | $2.9531^{+0.0916}_{-0.0658}$ | $0.321^{+0.242}_{-0.209}$ | $44.432^{+2.039}_{-5.404}$ | $89.59^{+0.28}_{-0.41}$
TOI-3082b | 428699140 | $1.926907^{+0.000128}_{-0.000134}$ | $2459309.1199^{+0.0010}_{-0.0010}$ | $0.0489^{+0.0020}_{-0.0019}$ | $3.6621^{+0.1464}_{-0.1448}$ | $0.355^{+0.247}_{-0.223}$ | $8.519^{+0.600}_{-1.286}$ | $87.63^{+1.54}_{-2.39}$
TOI-4308b | 144193715 | $9.151201^{+0.000036}_{-0.000037}$ | $2458333.4284^{+0.0026}_{-0.0029}$ | $0.0279^{+0.0014}_{-0.0015}$ | $2.4189^{+0.1195}_{-0.1333}$ | $0.384^{+0.259}_{-0.253}$ | $23.606^{+2.227}_{-3.906}$ | $89.07^{+0.64}_{-0.92}$
TOI-5803b | 466382581 | $5.383050^{+0.000207}_{-0.000200}$ | $2459802.7103^{+0.0004}_{-0.0005}$ | $0.0393^{+0.0015}_{-0.0014}$ | $3.2732^{+0.1251}_{-0.1194}$ | $0.349^{+0.223}_{-0.233}$ | $28.596^{+1.887}_{-3.423}$ | $89.30^{+0.48}_{-0.60}$

Figure 2: Phase-folded light curves of newly validated planetary systems.
Black line shows the best-fit model, blue dots are binned observations.

Figure 3: Phase-folded light curves of newly validated planetary systems.
Description same as Figure 2

Figure 4: Transmission spectroscopy values (Left) and emission spectroscopy
values (Right) for the newly validated planets, color-coded by their
equilibrium temperature. In each case the shaded regions indicate areas of
interest as identified by Kempton et al. (2018). Big dots represent the
planets amenable for transmission or emission spectroscopy.

###  5.1 TOI-139

TOI-139b is a sub-Neptune (2.4566 $R_{\earth}$) planet orbiting bright (Vmag =
10.55, Tmag = 9.36) star TOI-139 (0.70 $R_{\sun}$, 0.69 $M_{\sun}$), observed
in TESS sectors 1 and 28. It orbits the star at a distance of 0.11 AU with an
orbital period 11.07 days and having an equilibrium temperature 561.17 K.
’Alopeke and NIRC2 high resolution imaging showed no contaminating stellar
companion. The VESPA FPP and TRICERATOPS FPP and NFPP are listed in Table 2
calculated using four available contrast curve files. These FPP values are
consisting with the source of transit signal being on the target star. Using
the Chen & Kipping (2017) mass-radius relationship we predicted the mass 6.62
$M_{\earth}$. Based on this, resultant RV semi-amplitude is 2.43 m $s^{-1}$.
TSM and ESM are estimated as 68.30 and 3.18 respectively which are below the
recommended threshold of Kempton et al. (2018). So this target will not be
favourable for either transmission or emission spectroscopy.

###  5.2 TOI-277

TOI-277b is a sub-Neptune (3.0949 $R_{\earth}$) planet orbiting faint (Vmag =
13.63 , Tmag = 11.7315) star TOI-277 (0.52 $R_{\sun}$, 0.52 $M_{\sun}$),
observed in TESS sectors 3 and 30. It orbits the star at a distance of 0.033
AU with an orbital period 3.99 days and having an equilibrium temperature
739.90 K. Zorro, ’Alopeke and NIRI high resolution imaging showed no
contaminating stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP
are listed in Table 2 calculated using five available contrast curve files.
These FPP values are consisting with the source of transit signal being on the
target star. Using the Chen & Kipping (2017) mass-radius relationship we
predicted the mass 9.80 $M_{\earth}$. Based on this resultant RV semi-
amplitude is 6.10 m $s^{-1}$. TSM is estimated as 86.9548 which is comparable
but still below the threshold set by Kempton et al. (2018). However ESM is
predicted to be 10.34 above the 7.5, indicating that it is potentially a good
target for emission spectroscopy.

###  5.3 TOI-672

TOI-672b is a sub-Saturn or super-Neptune (5.26 $R_{\earth}$) planet orbiting
faint (Vmag = 13.57, Tmag = 11.67) star TOI-672 (0.54 $R_{\sun}$, 0.53
$M_{\sun}$), observed in TESS sectors 9, 10 and 36. It orbits the star at a
distance of 0.039 AU with an orbital period 3.63 days and having an
equilibrium temperature 676.15 K. Zorro high resolution imaging showed no
contaminating stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP
are listed in Table 2 calculated using two available contrast curve files.
These FPP values are consisting with the source of transit signal being on the
target star. Using the Chen & Kipping (2017) mass-radius relationship we
predicted the mass 24.15 $M_{\earth}$. Based on this resultant RV semi-
amplitude is 15.14 m $s^{-1}$. TSM and ESM are estimated as 134.15 and 22.93
respectively which are above the recommended threshold of Kempton et al.
(2018). So this target will be favourable for both transmission and emission
spectroscopy.

###  5.4 TOI-913

TOI-913b is a sub-Neptune (2.45 $R_{\earth}$) planet orbiting bright (Vmag =
10.45, Tmag = 9.62) star TOI-913 (0.73 $R_{\sun}$, 0.82 $M_{\sun}$), observed
in TESS sectors 12 and 13. It orbits the star at a distance of 0.083 AU with
an orbital period 11.09 days and having an equilibrium temperature 712 K.
Zorro high resolution imaging showed no contaminating stellar companion. The
VESPA FPP and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using
two available contrast curve files. These FPP values are consisting with the
source of transit signal being on the target star. Using the Chen & Kipping
(2017) mass-radius relationship we predicted the mass 6.60 $M_{\earth}$. Based
on this resultant RV semi-amplitude is 2.16 m $s^{-1}$. TSM and ESM are
estimated as 63.71 and 3.96 respectively which are below the recommended
threshold of Kempton et al. (2018). So this target will not be favourable for
either transmission or emission spectroscopy.

###  5.5 TOI-1410

TOI-1410b is a Neptune-like (3.24 $R_{\earth}$) planet orbiting bright (Vmag =
11.11, Tmag = 10.19) star TOI-1410 (0.78 $R_{\sun}$, 0.79 $M_{\sun}$),
observed in TESS sector 16. It orbits the star at a distance of 0.028 AU with
an orbital period 1.22 days and having an equilibrium temperature 1181.44 K.
PHARO, ’Alopeke and NIR2 high resolution imaging showed no contaminating
stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP are listed in
Table 2 calculated using four available contrast curve files. These FPP values
are consisting with the source of transit signal being on the target star.
Using the Chen & Kipping (2017) mass-radius relationship we predicted the mass
10.61 $M_{\earth}$. Based on this resultant RV semi-amplitude is 7.38 m
$s^{-1}$. TSM and ESM are estimated as 113.18 and 18.04 respectively which are
above the recommended threshold of Kempton et al. (2018). So this target will
be favourable for both transmission and emission spectroscopy.

###  5.6 TOI-1694

TOI-1694b is a sub-Saturn or super-Neptune (5.46 $R_{\earth}$) planet orbiting
bright (Vmag = 11.45, Tmag = 10.74) star TOI-1694 (0.82 $R_{\sun}$, 0.84
$M_{\sun}$), observed in TESS sectors 19 and 20. It orbits the star at a
distance of 0.039 AU with an orbital period 3.77 days and having an
equilibrium temperature 1136.57 K. ’Alopeke and NIRC2 high resolution imaging
showed no contaminating stellar companion. The VESPA FPP and TRICERATOPS FPP
and NFPP are listed in Table 2 calculated using three available contrast curve
files. These FPP values are consisting with the source of transit signal being
on the target star. Using the Chen & Kipping (2017) mass-radius relationship
we predicted the mass 25.71 $M_{\earth}$. Based on this resultant RV semi-
amplitude is 11.81 m $s^{-1}$. TSM and ESM are estimated as 125.91 and 25.89
respectively which are above the recommended threshold of Kempton et al.
(2018). So this target will be favourable for both transmission and emission
spectroscopy.

###  5.7 TOI-1801

TOI-1801b is a super-Earth (2.08 $R_{\earth}$) planet orbiting bright (Vmag =
11.58, Tmag = 9.85), metal-poor ([Fw/H] = -0.7186 $\pm$ 0.1) star TOI-1801
(0.55 $R_{\sun}$, 0.54 $M_{\sun}$), observed in TESS sectors 22 and 49. It
orbits the star at a distance of 0.077 AU with an orbital period 10.64 days
and having an equilibrium temperature 490.47 K. ’Alopeke and NIRC2 high
resolution imaging showed no contaminating stellar companion. The VESPA FPP
and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using three
available contrast curve files. These FPP values are consisting with the
source of transit signal being on the target star. Using the Chen & Kipping
(2017) mass-radius relationship we predicted the mass 5.02 $M_{\earth}$. Based
on this resultant RV semi-amplitude is 2.19 m $s^{-1}$. TSM and ESM are
estimated as 70.17 and 2.77 respectively which are below the recommended
threshold of Kempton et al. (2018). So this target will not be favourable for
either transmission or emission spectroscopy.

###  5.8 TOI-1853

TOI-1853b is a Neptune-like (3.64 $R_{\earth}$) planet orbiting moderately
bright (Vmag = 12.178, Tmag =11.37) star TOI-1853 (0.84 $R_{\sun}$, 0.82
$M_{\sun}$), observed in TESS sector 50. It orbits the star at a distance of
0.023 AU with an orbital period 1.24 days and having an equilibrium
temperature 1510.96 K. It is a hottest planet validated in this project.
’Alopeke and NIRC2 high resolution imaging showed no contaminating stellar
companion. The VESPA FPP and TRICERATOPS FPP and NFPP are listed in Table 2
calculated using three available contrast curve files. These FPP values are
consisting with the source of transit signal being on the target star. Using
the Chen & Kipping (2017) mass-radius relationship we predicted the mass 12.89
$M_{\earth}$. Based on this resultant RV semi-amplitude is 8.73 m $s^{-1}$.
TSM is estimated as 78.28 which is slightly below the threshold set by Kempton
et al. (2018). However ESM is predicted to be 13.57 above the 7.5, indicating
that it is potentially a good target for emission spectroscopy.

###  5.9 TOI-2018

TOI-2018b is a sub-Neptune (2.29 $R_{\earth}$) planet orbiting bright (Vmag =
10.25, Tmag = 8.96) star TOI-2018 (0.62 $R_{\sun}$, 0.66 $M_{\sun}$), observed
in TESS sectors 24 and 51. It orbits the star at a distance of 0.064 AU with
an orbital period 7.44 days and having an equilibrium temperature 652.44 K.
’Alopeke, PHARO and ShARCS high resolution imaging showed no contaminating
stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP are listed in
Table 2 calculated using five available contrast curve files. These FPP values
are consisting with the source of transit signal being on the target star.
Using the Chen & Kipping (2017) mass-radius relationship we predicted the mass
5.86 $M_{\earth}$. Based on this resultant RV semi-amplitude is 2.53 m
$s^{-1}$. TSM and ESM are estimated as 116.93 and 7.56 respectively which are
above the recommended threshold of Kempton et al. (2018). So this target will
be favourable for both transmission and emission spectroscopy.

###  5.10 TOI-2134

TOI-2134b is a sub-Neptune (2.96 $R_{\earth}$) planet orbiting bright (Vmag =
8.93, Tmag = 7.79) star TOI-2134 (0.77 $R_{\sun}$, 0.69 $M_{\sun}$), observed
in TESS sectors 26, 40, 52, 53 and 54. It orbits the star at a distance of
0.084 AU with an orbital period 9.23 days and having an equilibrium
temperature 665.25 K. PHARO high resolution imaging showed no contaminating
stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP are listed in
Table 2 calculated using one available contrast curve file. These FPP values
are consisting with the source of transit signal being on the target star.
Using the Chen & Kipping (2017) mass-radius relationship we predicted the mass
9.09 $M_{\earth}$. Based on this resultant RV semi-amplitude is 3.55 m
$s^{-1}$. TSM and ESM are estimated as 181.15 and 13.13 respectively which are
above the recommended threshold of Kempton et al. (2018). So this target will
be favourable for both transmission and emission spectroscopy.

###  5.11 TOI-2194

TOI-2194b is a super-Earth (1.99 $R_{\earth}$) planet orbiting bright (Vmag =
8.42, Tmag = 7.42), metal-poor ([Fw/H] = -0.3720 $\pm$ 0.1) star TOI-2194
(0.69 $R_{\sun}$, 0.74 $M_{\sun}$), observed in TESS sector 27. It orbits the
star at a distance of 0.10 AU with an orbital period 15.34 days and having an
equilibrium temperature 590.88 K. HRCam high resolution imaging showed no
contaminating stellar companion. The VESPA FPP and TRICERATOPS FPP and NFPP
are listed in Table 2 calculated using one available contrast curve file.
These FPP values are consisting with the source of transit signal being on the
target star. Using the Chen & Kipping (2017) mass-radius relationship we
predicted the mass 4.62 $M_{\earth}$. Based on this resultant RV semi-
amplitude is 1.45 m $s^{-1}$. TSM is estimated as 131.023 which is above the
threshold of second quartile suggested by Kempton et al. (2018), that makes it
a good target for transmission spectroscopy. In other hand ESM is 5.45 which
is comparable but still below 7.5. So emission spectroscopy would be
challenging.

###  5.12 TOI-2443

TOI-2443b is a sub-Neptune (2.77 $R_{\earth}$) planet orbiting bright (Vmag =
9.51, Tmag = 8.29) star TOI-2443 (0.73 $R_{\sun}$, 0.66 $M_{\sun}$), observed
in TESS sector 31. It orbits the star at a distance of 0.089 AU with an
orbital period 15.67 days and having an equilibrium temperature 600.83 K. This
is the coolest planet validated in this project. ’Alopeke and PHARO high
resolution imaging showed no contaminating stellar companion. The VESPA FPP
and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using three
available contrast curve files. These FPP values are consisting with the
source of transit signal being on the target star. Using the Chen & Kipping
(2017) mass-radius relationship we predicted the mass 8.13 $M_{\earth}$. Based
on this resultant RV semi-amplitude is 2.74 m $s^{-1}$. TSM and ESM are
estimated as 132.89 and 8.28 respectively which are above the recommended
threshold of Kempton et al. (2018). So this target will be favourable for both
transmission and emission spectroscopy.

###  5.13 TOI-2459

TOI-2459b is a sub-Neptune (2.95 $R_{\earth}$) planet orbiting bright (Vmag =
10.77, Tmag = 9.39) star TOI-2459 (0.67 $R_{\sun}$, 0.66 $M_{\sun}$), observed
in TESS sectors 5, 6, 32 and 33. It orbits the star at a distance of 0.14 AU
with an orbital period 19.10 days and having an equilibrium temperature 445 K.
high resolution imaging showed no contaminating stellar companion. The VESPA
FPP and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using one
available contrast curve file. These FPP values are consisting with the source
of transit signal being on the target star. Using the Chen & Kipping (2017)
mass-radius relationship we predicted the mass 9.05 $M_{\earth}$. Based on
this resultant RV semi-amplitude is 2.85 m $s^{-1}$. TSM and ESM are estimated
as 76.04 and 2.46 respectively which are below the recommended threshold of
Kempton et al. (2018). So this target will not be favourable for either
transmission or emission spectroscopy.

###  5.14 TOI-3082

TOI-3082b is a Neptune-like (3.66 $R_{\earth}$) planet orbiting faint (Vmag =
12.93, Tmag = 11.77) star TOI-3082 (0.68 $R_{\sun}$, 0.66 $M_{\sun}$),
observed in TESS sectors 37. It orbits the star at a distance of 0.027 AU with
an orbital period 1.93 days and having an equilibrium temperature 1032.78 K.
The VESPA FPP and TRICERATOPS FPP and NFPP are listed in Table 2 calculated
without using any contrast curve file. These FPP values are consisting with
the source of transit signal being on the target star. Using the Chen &
Kipping (2017) mass-radius relationship we predicted the mass 13.04
$M_{\earth}$. Based on this resultant RV semi-amplitude is 8.79 m $s^{-1}$.
TSM is estimated as 78.37 which is below the threshold set by Kempton et al.
(2018). However ESM is predicted to be 13.37 above the 7.5, indicating that it
is potentially a good target for emission spectroscopy.

###  5.15 TOI-4308

TOI-4308b is a sub-Neptune (2.42 $R_{\earth}$) planet orbiting bright (Vmag =
11.25, Tmag = 10.34) star TOI-4608 (0.79 $R_{\sun}$, 0.9 $M_{\sun}$), observed
in TESS sector 1. It orbits the star at a distance of 0.087 AU with an orbital
period 9.15 days and having an equilibrium temperature 763.05 K. HRCam high
resolution imaging showed no contaminating stellar companion. The VESPA FPP
and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using one
available contrast curve file. These FPP values are consisting with the source
of transit signal being on the target star. Using the Chen & Kipping (2017)
mass-radius relationship we predicted the mass 6.45 $M_{\earth}$. Based on
this resultant RV semi-amplitude is 2.11 m $s^{-1}$. TSM and ESM are estimated
as 39.68 and 2.48 respectively which are below the recommended threshold of
Kempton et al. (2018). So this target will not be favourable for either
transmission or emission spectroscopy.

###  5.16 TOI-5803

TOI-5803b is a sub-Neptune (3.27 $R_{\earth}$) planet orbiting bright (Vmag =
10.65, Tmag = 9.94) star TOI-5803 (0.76 $R_{\sun}$, 0.87 $M_{\sun}$), observed
in TESS sector 55. It orbits the star at a distance of 0.10 AU with an orbital
period 5.38 days and having an equilibrium temperature 678.87 K. HRCam high
resolution imaging showed no contaminating stellar companion. The VESPA FPP
and TRICERATOPS FPP and NFPP are listed in Table 2 calculated using one
available contrast curve file. These FPP values are consisting with the source
of transit signal being on the target star. Using the Chen & Kipping (2017)
mass-radius relationship we predicted the mass 10.78 $M_{\earth}$. Based on
this resultant RV semi-amplitude is 4.31 m $s^{-1}$. TSM and ESM are estimated
as 69.70 and 4.55 respectively which are below the recommended threshold of
Kempton et al. (2018). So this target will not be favourable for either
transmission or emission spectroscopy.

##  6 Likely Planets and Not Validated Candidates

In Table 2, we listed Likely Planets as well as Not Validated candidates. We
considered targets Likely planet for which one of the FPP calculators produced
a planet-like signal and another produced a likely planet-like signal. (in the
case of TRICERATOPS, the target is a likely planet if FPP is FPP ¡ 0.5 and
NFPP ¡ 10-03 (Giacalone & Dressing, 2020)). We identified three such targets
that can be followed up further to establish their planetary nature. These
targets are,

  * •

TOI-1732

This target was observed in two sectors, 20 and 47. As can be seen from Table
2, the results from both the VESPA and TRICERATOPS FPP calculators indicate
that sector 20 produced a signal with a FPP consistent with a false positive,
while sector 47 produced a signal with a FPP consistent with a planet-like
signal. Given this discrepancy, further follow-up observations utilizing high-
resolution radial velocity data would be necessary to confirm the planetary
nature of this target.

  * •

TOI-2200

This target was observed in twelve sectors: 27, 28, 29, 30, 31, 32, 33, 34,
36, 37, 38, and 39. VESPA FPP calculation for every sector suggests that
TOI-2200 is a planet, while TRICERATOPS gives a likely planet scenario. Also,
we do not have any high-resolution images for this target. So further follow-
up of Spackle or Adaptive Optics (AO) imaging and radial velocity data is
needed to make any comment about its planetary nature.

  * •

TOI-5704

This target was observed in two sectors: 22 and 48. Refer to Table 2, VESPA
gives false positive like FPP while TRICERATOPS gives planet like FPP. We do
not have any high-resolution images for this target. So further follow-up of
Spackle or Adaptive Optics (AO) imaging and radial velocity data is needed.

Below are the list of not validated planets.

  * •

Candidates which failed both VESPA and TRICERATOPS threshold.

    * –

TOI 323

    * –

TOI 2408

    * –

TOI 3896

    * –

TOI 3913

    * –

TOI 4090

    * –

TOI 5584

  * •

Candidates which failed either of the threshold.

    * –

TOI 815 (Noisy signal with 1 % False Alarm Probability.)

    * –

TOI 1179 (TRICERATOPS has detected blended eclipsing binary.)

    * –

TOI 3568

  * •

Other candidates

    * –

TOI 493 (VESPA gave both planet-like and false positive like FPP for various
sectors, while TRICERATOPS gave a false positive like FPP.)

    * –

TOI 1180 (VESPA and TRICERATOPS both gave planet-like and false positive like
FPP)

##  7 Conclusions

In this study, out of the 30 initial candidates selected for examination, 16
new TESS exoplanetary systems have been verified, resulting in a validation
rate of 53.33%. Among these recently validated planets, there are several
intriguing targets that worthy for further investigation into their
atmospheres. For example, based on the estimated Transmission Spectroscopy
Metrics (TSM) values, TOI-2194b is considered a promising candidate for the
investigation of its atmosphere via transmission spectroscopy. Similarly,
TOI-277b, TOI-1853b, and TOI-3082b are considered to be optimal targets for
investigating via emission spectroscopy, as per their estimated Emission
Spectroscopy Metrics (ESM) values. Additionally, based on the TSM and ESM
values, TOI-672b, TOI-1410b, TOI-1694b, TOI-2018b, TOI-2134b, and TOI-2443b
are considered to be promising candidates for the investigation of their
atmospheres via both transmission and emission spectroscopy. Furthermore, we
have identified three potential planets that would benefit from further
investigation through the use of radial velocity and high-resolution imaging
techniques in order to establish their planetary nature with a high degree of
certainty. These investigations would help to reveal more about the properties
and behavior of these exoplanets and provide insights into the formation and
evolution of planetary systems.

##  8 Acknowledgements

M.V.G. and I.A.S. acknowledge the support of Ministry of Science and Higher
Education of the Russian Federation under the grant 075-15-2020-780
(N13.1902.21.0039). Observations in the paper made use of the High-Resolution
Imaging instruments ‘Alopeke and Zorro. ‘Alopeke and Zorro were funded by the
NASA Exoplanet Exploration Program and built at the NASA Ames Research Center
by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke
and Zorro was mounted on the Gemini North and South telescope of the
international Gemini Observatory, a program of NSF’s NOIRLab, which is managed
by the Association of Universities for Research in Astronomy (AURA) under a
cooperative agreement with the National Science Foundation. on behalf of the
Gemini partnership: the National Science Foundation (United States), National
Research Council (Canada), Agencia Nacional de Investigación y Desarrollo
(Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina),
Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and
Korea Astronomy and Space Science Institute (Republic of Korea). This research
has made use of the Exoplanet Follow-up Observation Program (ExoFOP;
DOI:http://dx.doi.org/10.26134/ExoFOP5 (catalog 10.26134/ExoFOP5)) website,
which is operated by the California Institute of Technology, under contract
with the National Aeronautics and Space Administration under the Exoplanet
Exploration Program. This publication makes use of data products collected by
the TESS mission and obtained from the MAST data archive at the Space
Telescope Science Institute (STScI). The light curve and target pixel file
data used in this paper can be found in
http://dx.doi.org/10.17909/t9-nmc8-f686 (catalog 10.17909/t9-nmc8-f686).

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