TESS News and Results

Second transit of TOI-2180b, confirming the orbital period of 260.15764 ± 0.00045 days, time of conjunction BJD 2458830.76417 ± 0.00099.

Dalba et al. (2022) "The Refined Transit Ephemeris of TOI-2180 b"
https://iopscience.iop.org/article/10.3847/2515-5172/ac64fd

Super-Neptune on a low-eccentricity orbit around TOI-1710=TYC 4245-1009-1=BD+76°227

"A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE and HARPS-N"
https://arxiv.org/abs/2204.08984

TOI-1696 and TOI-2136: Constraining the Masses of Two Mini-Neptunes with HPF
https://arxiv.org/abs/2204.09063

The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc

Quote :

We report the discovery of a multi-planetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of Rb = 1.240±0.023 R⊕, a mass of Mb = 2.14±0.34 M⊕, and a bulk density of ρb = 6.2±1.0 g cm−3, and HD 260655 c, with a period of 5.71 d, a radius of Rc = 1.533+0.051−0.046 R⊕, a mass of Mc = 3.09±0.48 M⊕, and a bulk density of ρc = 4.7+0.9−0.8 g cm−3. The planets were detected in transit by the TESS mission and confirmed independently with archival and new precise radial velocities obtained with the HIRES and CARMENES instruments since 1998 and 2016, respectively. At a distance of 10 pc, HD 260655 becomes the fourth closest known multi-transiting planet system after HD 219134, LTT 1445 A, and AU Mic. Due to the apparent brightness of the host star (J = 6.7 mag), both planets are among the most suitable rocky worlds known today for atmospheric studies with the JWST, both in transmission and emission.

Mass measurements for the four planets orbiting TOI-1246, plus an unconfirmed fifth RV-only planet in a 93.8-day orbit:

Turtelboom et al. "The TESS-Keck Survey. XI. Mass Measurements for Four Transiting sub-Neptunes orbiting K dwarf TOI-1246"
https://arxiv.org/abs/2204.11895

A mini-Neptune around the primary of a ~56 au G+M binary:

Zhou et al. "A Mini-Neptune from TESS and CHEOPS Around the 120 Myr Old AB Dor member HIP 94235"
https://arxiv.org/abs/2204.11975

TESS data used to find possible TTVs in WASP-161b:

Yang & Chary "Tentative Evidence for Transit Timing Variations of WASP-161b"
https://arxiv.org/abs/2204.12306

Three more non-transiting planets in TOI-500 system

A low-eccentricity migration pathway for a 13-h-period Earth analogue in a four-planet system

Quote :

It is commonly accepted that exoplanets with orbital periods shorter than 1 day, also known as ultra-short period (USP) planets, formed further out within their natal protoplanetary disk, before migrating to their current-day orbits via dynamical interactions. One of the most accepted theories suggests a violent scenario involving high-eccentricity migration followed by tidal circularization. Here, we present the discovery of a four planet system orbiting the bright (V=10.5) K6 dwarf star TOI-500. The innermost planet is a transiting, Earth-sized USP planet with an orbital period of ∼ 13 hours, a mass of 1.42 ± 0.18 M⊕, a radius of 1.166^+0.061_−0.058 R⊕, and a mean density of 4.89^+1.03_−0.88 gcm⁻³. Via Doppler spectroscopy, we discovered that the system hosts three outer planets on nearly circular orbits with periods of 6.6, 26.2, and 61.3d and minimum masses of 5.03 ± 0.41 M⊕, 33.12 ± 0.88 M⊕ and 15.05^+1.12_−1.11 M⊕, respectively. The presence of both a USP planet and a low-mass object on a 6.6-day orbit indicates that the architecture of this system can be explained via a scenario in which the planets started on low-eccentricity orbits, then moved inwards through a quasi-static secular migration. Our numerical simulations show that this migration channel can bring TOI-500 b to its current location in 2 Gyrs, starting from an initial orbit of 0.02au. TOI-500 is the first four planet system known to host a USP Earth analog whose current architecture can be explained via a non-violent migration scenario.

Edasich wrote:

A low-eccentricity migration pathway for a 13-h-period Earth analogue in a four-planet system

Well that certainly is an interesting usage of the term "Earth analogue".

From the title I was expecting a planetary system around a white or brown dwarf.

I'm posting this here because GJ 412, either A or B (WX UMa), is listed by TESS as candidate exoplanet host.

Radio masers on WX UMa: hints of a Neptune-sized planet, or magnetospheric reconnection?

Quote :

The nearby M dwarf WX UMa has recently been detected at radio wavelengths with LOFAR. The combination of its observed brightness temperature and circular polarisation fraction suggests that the emission is generated via the electron-cyclotron maser instability. Two distinct mechanisms have been proposed to power such emission from low-mass stars: either a sub-Alfvénic interaction between the stellar magnetic field and an orbiting planet, or reconnection at the edge of the stellar magnetosphere. In this paper, we investigate the feasibility of both mechanisms, utilising the information about the star's surrounding plasma environment obtained from modelling its stellar wind. Using this information, we show that a Neptune-sized exoplanet with a magnetic field strength of 10-100 G orbiting at ~0.034 au can accurately reproduce the observed radio emission from the star, with corresponding orbital periods of 7.4 days. Due to the stellar inclination, a planet in an equatorial orbit is unlikely to transit the star. While such a planet could induce radial velocity semi-amplitudes from 7 to 396 m s^-1, it is unlikely that this signal could be detected with current techniques due to the activity of the host star. The application of our planet-induced radio emission model here illustrates its exciting potential as a new tool for identifying planet-hosting candidates from long-term radio monitoring. We also develop a model to investigate the reconnection-powered emission scenario. While this approach produces less favourable results than the planet-induced scenario, it nevertheless serves as a potential alternative emission mechanism which is worth exploring further.

Three more planets

TOI-2046b, TOI-1181b and TOI-1516b, three new hot Jupiters from TESS: planets orbiting a young star, a subgiant and a normal star

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We present the confirmation and characterization of three hot Jupiters, TOI-1181b, TOI-1516b, and TOI-2046b, discovered by the TESS space mission. The reported hot Jupiters have orbital periods between 1.4 and 2.05 days. The masses of the three planets are 1.18±0.14 MJ, 3.16±0.12 MJ, and 2.30 ±0.28 MJ, for TOI-1181b, TOI-1516b, and TOI-2046b, respectively. The stellar host of TOI-1181b is a F9IV star, whereas TOI-1516b and TOI-2046b orbit F main sequence host stars. The ages of the first two systems are in the range of 2-5 Gyrs. However, TOI-2046 is among the few youngest known planetary systems hosting a hot Jupiter, with an age estimate of 100-400 Myrs. The main instruments used for the radial velocity follow-up of these three planets are located at Ondřejov, Tautenburg and McDonald Observatory, and all three are mounted on 2-3 meter aperture telescopes, demonstrating that mid-aperture telescope networks can play a substantial role in the follow-up of gas giants discovered by TESS and in the future by PLATO

The Discovery of a Planetary Companion Interior to Hot Jupiter WASP-132 b
https://arxiv.org/abs/2205.02501

Sirius_Alpha wrote:

The Discovery of a Planetary Companion Interior to Hot Jupiter WASP-132 b
https://arxiv.org/abs/2205.02501

Astonishing!

Another Shipment of Six Short-Period Giant Planets from TESS
https://arxiv.org/abs/2205.05709

HD 28109 hosts a trio of transiting Neptunian planets including a near-resonant pair, confirmed by ASTEP from Antarctica

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We report on the discovery and characterisation of three planets orbiting the F8 star HD~28109, which sits comfortably in \tess's continuous viewing zone. The two outer planets have periods of 56.0067±0.0003 days and 84.2597+0.0010−0.0008 days, which implies a period ratio very close to that of the first-order 3:2 mean motion resonance, exciting transit timing variations (TTVs) of up to 60mins. These two planets were first identified by \tess, and we identified a third planet in the \textcolor{black}{\tess photometry} with a period of 22.8911±0.0004 days. We confirm the planetary nature of all three planetary candidates using ground-based photometry from Hazelwood, ASTEP and LCO, including a full detection of the ∼9h transit of HD~28109 c from Antarctica. The radii of the three planets are \textcolor{black}{Rb=2.199+0.098−0.10 R⊕, Rc=4.23±0.11 R⊕ and Rd=3.25±0.11 R⊕}; we characterise their masses using TTVs and precise radial velocities from ESPRESSO and HARPS, and find them to be Mb=18.5+9.1−7.6 M⊕, Mc=7.9+4.2−3.0 M⊕ and Md=5.7+2.7−2.1 M⊕, making planet b a dense, massive planet while c and d are both under-dense. We also demonstrate that the two outer planets are ripe for atmospheric characterisation using transmission spectroscopy, especially given their position in the CVZ of JWST. The data obtained to date are consistent with resonant (librating) and non-resonant (circulating) solutions; additional observations will show whether the pair is actually locked in resonance or just near-resonant.

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

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We report the discovery of ten short-period giant planets (TOI-2193A b, TOI-2207 b, TOI-2236 b, TOI-2421 b, TOI-2567 b, TOI-2570 b, TOI-3331 b, TOI-3540A b, TOI-3693 b, TOI-4137 b). All of the planets were identified as planet candidates based on periodic flux dips observed by NASA's Transiting Exoplanet Survey Satellite (TESS). The signals were confirmed to be from transiting planets using ground-based time-series photometry, high angular resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The ten newly discovered planets orbit relatively bright F and G stars (G<12.5,~Teff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10~days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421 b is notable for being a Saturn-mass planet and TOI-2567 b for being a ``sub-Saturn'', with masses of 0.322±0.073 and 0.195±0.030 Jupiter masses, respectively. In most cases, we have little information about the orbital eccentricities. Two exceptions are TOI-2207 b, which has an 8-day period and a detectably eccentric orbit (e=0.17±0.05), and TOI-3693 b, a 9-day planet for which we can set an upper limit of e<0.052. The ten planets described here are the first new planets resulting from an effort to use TESS data to unify and expand on the work of previous ground-based transit surveys in order to create a large and statistically useful sample of hot Jupiters.

Quote :

6) Some additions to A-type stars: TOI-1107, TOI-629, TOI-1982 and TOI-2336 (massive planet the former, BDs the latter three)

Exoplanet and brown dwarfs transiting A-F type stars

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The detection and characterization of exoplanets around a broad range of host stars, including massive A-F stars, is essential to investigate and constrain the impact of stellar mass on planet properties. However, planets around hot massive hosts are still relatively unexplored in radial velocity (RV) surveys because of the small number of stellar lines that are usually broadened and blended by stellar rotation and jitter. As a result, the available information about the formation and evolution of planets around hot stars is limited. Our observing program focuses on bright (V<12) giant (>7 Re) planet and brown dwarf candidates orbiting stars with effective temperatures above 6200 K  identified from the TESS mission. For the confirmation of their planetary nature and the determination of their mass and orbital properties, we use RVs and spectra mainly from CORALIE and other instruments as part of the TESS Follow-up Observing Program. For some fast rotating stars that require higher precision and efficiency we foresee to use HARPS. We present our global statistical analysis of TESS candidates transiting early-type stars and the detection of a massive planet, TOI-1107, and three new brown dwarfs, TOI-629, TOI-1982 and TOI-2336.

Now published but showing TOI-2543 in place of TOI-2336.

Three new brown dwarfs and a massive hot Jupiter revealed by TESS around early-type stars

Quote :

The detection and characterization of exoplanets and brown dwarfs (BDs) around massive AF-type stars is essential to investigate and constrain the impact of stellar mass on planet properties. However, such targets are still poorly explored in radial velocity (RV) surveys because they only feature a small number of stellar lines and those are usually broadened and blended by stellar rotation as well as stellar jitter. As a result, the available information about the formation and evolution of planets and BDs around hot stars is limited. We aim to increase the sample and precisely measure the masses and eccentricities of giant planets and BDs transiting AF-type stars detected by the Transiting Exoplanet Survey Satellite (TESS). We followed bright (V < 12 mag) stars with Teff > 6200 K that host giant companions (R > 7 R⊕) using ground-based photometric observations as well as high precision RV measurements from the CORALIE, CHIRON, TRES, FEROS, and MINERVA-Australis spectrographs. In the context, we present the discovery of three BD companions, TOI-629b, TOI-1982b, and TOI-2543b, and one massive planet, TOI-1107b. From the joint analysis we find the BDs have masses between 66 and 68 M_Jup, periods between 7.54 and 17.17 days, and radii between 0.95 and 1.11 R_Jup. The hot Jupiter TOI-1107b has an orbital period of 4.08 days, a radius of 1.30 RJup, and a mass of 3.35 M_Jup. As a by-product of this program, we identified four low-mass eclipsing components (TOI-288b, TOI-446b, TOI-478b, and TOI-764b). Both TOI-1107b and TOI-1982b present an anomalously inflated radius with respect to the age of these systems. TOI-629 is among the hottest stars with a known transiting brown dwarf. TOI-629b and TOI-1982b are among the most eccentric brown dwarfs.

Binary companions to known and new TOIs
Determining Which Binary Component Hosts the TESS Transiting Planet

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The NASA TESS mission has discovered many transiting planets orbiting bright nearby stars, and high-resolution imaging studies have revealed that a number of these exoplanet hosts reside in binary or multiple star systems. In such systems, transit observations alone cannot determine which star in the binary system actually hosts the orbiting planet. The knowledge of which star the planet orbits is necessary for determining accurate physical properties for the planet, especially its true radius and mean bulk density. We derived the mean stellar densities for the components of 23 binary systems using the light curve transit shape and the binary flux ratio from speckle imaging, then tested the consistency with stellar models to determine which component is the host star. We found that 70% of the TESS transiting planets in our sample orbit the primary star.

New TOIs: TOI-159, 295, 309, 322, 462, 487, 489, 601, 697*, 931, 1217, 1267, 1287, 1288*, 1307, 1409 and 1740.

Known TOIs: TOI-141* (=HD 213885), 172, 194 (=WASP-20 Ab), 264 (=WASP-72 b), 492 (=HAT-P-50 b), 640 and 1267 (=Kepler-14 Ab).

(*) = triple systems

Characterization of TOI-1807 b

The GAPS Programme with HARPS-N at TNG. XXXVII. A precise density measurement of the young ultra-short period planet TOI-1807 b

Quote :

Great strides have been made in recent years in the understanding of the mechanisms involved in the formation and evolution of planetary systems; despite this, many observational facts still do not have an explanation. A great contribution to the study of planetary formation processes comes from the study of young, low-mass planets, with short orbital periods. In the last years, the TESS satellite has identified many planets of this kind, and their characterization is mandatory to understand how they formed and evolved. Within the framework of the GAPS project, we performed the validation and characterization of the ultra-short period planet (USPP) TOI-1807b, orbiting its young host star BD+39 2643 (~300 Myr) in only 13 hours. This is the youngest USPP discovered so far. Thanks to a joint modeling of the stellar activity and planetary signals in the TESS light curve and in HARPS-N radial-velocity measurements, combined with accurate estimation of stellar parameters, we validated the planetary nature of TOI-1807b and measured its orbital and physical parameters. By using astrometric, photometric, and spectroscopic observations we found that BD+39 2643 is a young, active K dwarf star, member of a 300+/-80 Myr old moving group and that it rotates in Prot=8.8+/-0.1 days. This star hosts an USPP with an orbital period of only P_b=0.54937+/-0.00001 d. Thanks to the exquisite photometric and spectroscopic series, and the accurate information on the stellar activity, we measured both the radius and the mass of TOI-1807b with high precision, obtaining R_b=1.37+/-0.09 R_Earth and M_b=2.57+/-0.50 M_Earth. These planet parameters correspond to a rocky planet with an Earth-like density and no extended H/He envelope. From the analysis of the age-R_P distribution for planets with well measured ages, we inferred that TOI-1807b may have already lost a large part of its atmosphere during its 300 Myr life.

Pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets In TESS Primary Mission Photometry

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Kepler's short-period exoplanet population has revealed evolutionary features such as the Radius Valley and the Hot Neptune desert that are likely sculpted by atmospheric loss over time. These findings suggest that the primordial planet population is different from the Gyr-old Kepler population, and motivates exoplanet searches around young stars. Here, we present pterodactyls , a data reduction pipeline specifically built to address the challenges in discovering exoplanets around young stars and to work with TESS Primary Mission 30-min cadence photometry, since most young stars were not pre-selected TESS 2-min cadence targets. pterodactyls builds on publicly available and tested tools in order to extract, detrend, search, and vet transiting young planet candidates. We search five clusters with known transiting planets: Tucana-Horologium Association, IC 2602, Upper Centaurus Lupus, Ursa Major and Pisces Eridani. We show that pterodactyls recovers seven out of the eight confirmed planets and one out of the two planet candidates, most of which were initially detected in 2-min cadence data. For these clusters, we conduct injection-recovery tests to characterize our detection efficiency, and compute an intrinsic planet occurrence rate of 49+-20% for sub-Neptunes and Neptunes (1.8-6 Re) within 12.5 days, which is higher than Kepler's Gyr-old occurrence rates of 6.8+-0.3%. This potentially implies that these planets have shrunk with time due to atmospheric mass loss. However, a proper assessment of the occurrence of transiting young planets will require a larger sample unbiased to planets already detected. As such, pterodactyls will be used in future work to search and vet for planet candidates in nearby clusters and moving groups.

TESS Hunt for Young and Maturing Exoplanets (THYME) VII : Membership, rotation, and lithium in the young cluster Group-X and a new young exoplanet

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The public, all-sky surveys Gaia and TESS provide the ability to identify new young associations and determine their ages. These associations enable study of planetary evolution by providing new opportunities to discover young exoplanets. A young association was recently identified by Tang et al. and F{ü}rnkranz et al. using astrometry from Gaia (called "Group-X" by the former). In this work, we investigate the age and membership of this association; and we validate the exoplanet TOI 2048 b, which was identified to transit a young, late G dwarf in Group-X using photometry from TESS. We first identified new candidate members of Group-X using Gaia EDR3 data. To infer the age of the association, we measured rotation periods for candidate members using TESS data. The clear color--period sequence indicates that the association is the same age as the 300±50 Myr-old NGC 3532. We obtained optical spectra for candidate members that show lithium absorption consistent with this young age. Further, we serendipitously identify a new, small association nearby Group-X, which we call MELANGE-2. Lastly, we statistically validate TOI 2048 b, which is 2.1±0.2 \rearth\ radius planet on a 13.8-day orbit around its 300 Myr-old host star.

At least two confirmed TOIs (in open clusters too) have been overlooked lately:

A Search for Exoplanets in Open Clusters and Young Associations based on TESS Objects of Interest

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We report the results of our search of planet candidates in Open Clusters and Young Stellar Associations based on the TESS Objects of Interest Catalog. We find one confirmed planet, one promising candidate, one brown dwarf, and three unverified planet candidates in a sample of 1229 Open Clusters from the second Gaia data release. We discuss individual planet-star systems based on their basic parameters, membership probability, and the observation notes from the ExoFOP-TESS website. We also find ten planet candidates (P > 95%) in Young Stellar Associations by using the BANYAN Σ Bayesian Algorithm. Among the ten candidates, five are known planet systems. We estimate the rotation periods of the host stars using the TESS light curves and estimate their ages based on gyrochronology. Two candidates with periodic variations are likely to be young planets, but their exact memberships to Young Stellar Associations remain unknown.

Quote :

The current TOI Catalog includes over 5000 young planet candidates nearby. We search for planets in 1229 Open Clusters based on the TOI catalog. We find one confirmed planet (TOI 837.01), one brown dwarf (TOI 681.01),one promising candidate (VPC+, TOI 1881.01), and three more unverified due to lack of data (TOI 4668.01, TOI 2538.01, TOI 581.01). For promising candidates, follow-up studies are possible with large telescopes.

About TOI-681, that is above hydrogen burning limit (88.7 M_Jup):

Populating the brown dwarf and stellar boundary: Five stars with transiting companions near the hydrogen-burning mass limit

A Hot Sub-Neptune in the Desert and a Temperate Super-Earth Around Faint M Dwarfs: Color Validation of TOI-4479b and TOI-2081b
http://arxiv.org/abs/2206.10643

Sirius_Alpha wrote:

The Longest Period TESS Planet Yet: A Sub-Neptune Transiting A Bright, Nearby K Dwarf Star
https://arxiv.org/abs/1901.00051

Quote :

The future of exoplanet science is bright, as TESS once again demonstrates with the discovery of its longest-period confirmed planet yet, located only 16 pc away. We hereby present HD 21749b (TOI 186.01), a sub-Neptune in a 36-day orbit around a bright (V = 8.1), nearby K4.5 dwarf. TESS measures HD21749b to be 2.84+0.26−0.22 R⊕, and combined archival and follow-up precision radial velocity data put the mass of the planet at 23.20+2.13−1.91 M⊕. HD 21749b is the longest-period TESS planet confirmed to date, and contributes to the TESS Level 1 Science Requirement of providing 50 transiting planets smaller than 4 R⊕ with measured masses. Furthermore, we report the discovery of TOI 186.02, a planet candidate with a 7.8-day period which, if confirmed, could become the first Earth-sized planet discovered by TESS. The HD21749 system is thus a prime candidate for comparative studies of planetary composition and architecture in multi-planet systems.

This brings planet count to 5,100 according to EPE. Actually the number is much higher accounting confirmed K2 and Kepler (and not only) planets published but not listed. But so be it...

Several binary companions to TESS objects of interest, some of which white dwarfs. In the sample also a WD companion to WASP-71 (TOI-388) and low-mass M dwarf to WASP-136 (TOI-2380)

Gaia Search for stellar Companions of TESS Objects of Interest III

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The latest results from our ongoing multiplicity study of (Community) TESS Objects of Interest are presented, using astro- and photometric data from the ESA-Gaia mission, to detect stellar companions of these stars and characterize their properties. A total of 124 binary and 7 hierarchical triple star systems were detected among 2175 targets, whose multiplicity was investigated in the course of our survey, which are located at distances closer than about 500pc around the Sun. The detected companions and the targets are located at the same distance and share a common proper motion, as expected for components of gravitationally bound stellar systems, as proven with their accurate Gaia EDR3 astrometry. The companions have masses in the range between about 0.09 and 2.5M⊙ and are most frequently found in the mass range between 0.15 and 0.8M⊙. The companions exhibit projected separations to the targets between about 50 to 9700au and their frequency is the highest and constant up to about 500au, while it decreases for larger projected separations. In addition to mainly mid M to early K dwarfs, 4 white dwarf companions were detected in this survey, whose true nature could be identified with their photometric properties.

Confirmation of the planet candidate TOI-1272.01 and discovery of a second non-transiting planet from doppler spectroscopy.

The TESS-Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-Mass Outer Companion around TOI-1272
http://arxiv.org/abs/2206.14327

The GAPS Programme at TNG XL: A puffy and warm Neptune-sized planet and an outer Neptune-mass candidate orbiting the solar-type star TOI-1422
https://arxiv.org/abs/2207.03293

Validated TESS exoplanets around K (sub)giant stars from a PhD thesis:

Detection and characterization of planets orbiting oscillating red-giant stars with NASA’s TESS mission

Quote :

Driven largely by multiple ground-based radial-velocity (RV) surveys and photometric space missions such as Kepler and K2, the discovery of new exoplanets has increased rapidly since the early 2000s. However, due to a target selection bias in favor of main-sequence stars, only a handful of transiting planets have been found orbiting evolved hosts. These planets, most of which are giants, hold important information regarding the formation and evolution of planetary systems. In this thesis, I sought to increase the sample of known giant planets orbiting red-giant stars, focusing on data from NASA's Transiting Exoplanet Survey Satellite (TESS) mission, and to improve their characterization. Specifically, I focused on close-in giant planets orbiting (preferably) oscillating low-luminosity red-giant branch (LLRGB) stars. To improve characterization, I developed a method to model planetary transits and stellar signals simultaneously, implementing Gaussian processes to model stellar granulation and the oscillations envelope in the time domain. My results show that the model enables time-domain asteroseismology, inferring the frequency of maximum oscillation amplitude, νmax, to within 1\%. The method's implementation is open-source and available to the community. Regarding the planet search, I assembled a pipeline, mostly comprised of third-party open-source software and explored a sample of ∼40,000 bright LLRGB stars in the southern hemisphere of TESS's field of view. The search identified four planet candidates, two of which are not currently known planets and orbit red-giant stars. Radial-velocity follow-up observations of both these candidates have tentatively confirmed their planetary nature. Finally, I also confirmed the planetary nature of an additional candidate, not part of the above sample, through RV observations.

Validated systems are TIC 394918211 (or TOI-4377) in Chamaeleon and TIC 204650483 in Hydra (aka HD 107244 or TOI-4551).

TESS Observations of Kepler systems with Transit Timing Variations

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We identify targets in the Kepler field that may be characterized by transit timing variations (TTVs) and are detectable by the Transiting Exoplanet Survey Satellite (TESS). Despite the reduced signal-to-noise ratio of TESS transits compared to Kepler, we recover 48 transits from 13 systems in Sectors 14, 15, 26, 40 and 41. We find strong evidence of a nontransiting perturber orbiting Kepler-396 (KOI-2672) and explore two possible cases of a third planet in that system that could explain the measured transit times. We update the ephemerides and mass constraints where possible at KOI-70 (Kepler-20), KOI-82 (Kepler-102), KOI-94 (Kepler-89), KOI-137 (Kepler-18), KOI-244 (Kepler-25), KOI-245 (Kepler-37), KOI-282 (Kepler-130), KOI-377 (Kepler-9), KOI-620 (Kepler-51), KOI-806 (Kepler-30), KOI-1353 (Kepler-289) and KOI-1783 (Kepler-1662).