Name Affiliation Title Abstract

ElianaAmazo-Gomez

Max Planck Institutefor Solar SystemResearch

ComprehensiveAnalysis ofSimultaneousPhotometric andSpectropolarimetricData in a YoungSun-like Star:Rotation Period,Variability, Activity& Magnetism.

Combined and simultaneous observations of high-precisionphotometric time-series acquired by TESS observatory andhigh-stability, high-accuracy measurements fromESO/HARPS telescope allow us to perform a robust stellarmagnetic-activity analysis. We retrieve information of thephotometric variability, rotation period and faculae/spotcoverage ratio from the gradient of the power spectra method(GPS). In addition magnetic field, chromospheric activity andradial velocity information are acquired from thespectropolarimetric observations. We aim to identify thepossible correlations between these different observables andplace our results in the context of the magnetic activitycharacterization in low-mass stars.

Tim Bedding University of SydneyAsteroseismologyof High-FrequencyDelta Scuti Starswith TESS

Asteroseismology is a powerful tool for probing stellarinteriors and has been applied with great success to manyclasses of stars. It is most effective when there are manyobserved modes that can be identified and compared withtheoretical models. Among evolved stars, the biggestadvances have come for red giants and white dwarfs. Amongmain-sequence stars, great results have been obtained for low-mass (Sun-like) stars and for hot high-mass stars. However, atintermediate masses (about 1.5 to 2.5 ), results from thelarge number of so-called delta Scuti pulsating stars havebeen very disappointing. The delta Scuti stars are verynumerous (about 2000 were detected in the Kepler field,mostly in long-cadence data). Many have a rich set ofpulsation modes but, despite years of effort, the identificationof the modes has proved extremely difficult. One problem isthat only a seemingly random subset of possible modes areexcited, making it difficult to identify a regular pattern. Thisis compounded by rapid rotation and by the low radial orders,both of which tend to spoil the regularity. TESS observationshave finally led to a breakthrough. We have focussed on thehigher-frequency delta Scuti stars (above about 30 c/d), sincethese seemed to offer the best hope for identifying regularpatterns. The large set of TESS short-cadence light curves areideally suited to this. We have been able to identify dozens ofdelta Scuti stars with very regular pulsation spectra. For thefirst time, we can identify the modes (assigning n and lvalues) and compare the frequencies with theoretical models.These results will enable TESS to open up intermediate-massstars to the power of asteroseismology, allowing us to placestrong constraints on masses, ages and internal rotation. Weare currently preparing a paper for Nature or NatureAstronomy.

FrancoisBouchy

Geneva Observatory Mass Measurementwith ESPRESSO ofRocky WorldsDetected by TESS

TESS follow-up efforts using high-precision spectrographsare ongoing to characterize transiting planets with radii below

, however still with a limited scope: only the moremassive planets on shorter-period orbits are amenable torobust mass measurements. ESPRESSO is the new highly-stabilized and high-resolution spectrograph in operation atESO/VLT since last September. ESPRESSO represents abreakthrough in this field: its 2-magnitude gain and improvedradial velocity precision with respect to HARPS-likeinstruments allows a thorough exploration of the rocky worldpopulation with radii below detected by TESS. We

will present an overview of the ESPRESSO performances,describe the TESS targets selected for the ESPRESSOGuarantee Time Observing program, and the first resultsobtained.

Luke Bouma Princeton University The Early Arrivalof WASP-4b

In a search for timing anomalies in previously known hotJupiter systems, one object has stood out: WASP-4b transited

seconds earlier than expected, based on datastretching back to 2007. Its orbital period also appears to beshrinking, by milliseconds per year. The periodchange could be caused by tidal orbital decay, apsidalprecession, or the gravitational influence of a third body.Confirming whether any of these processes are at work wouldbe interesting because it would teach us about the forces thatgovern the lives and potentially ultimate fates of hot Jupiters.Though more data are needed to understand the specific caseof WASP-4b, further TESS observations should enablebroader timing studies of the hot Jupiter population. Suchstudies will likely improve our understanding of both planet-planet and planet-star interactions.

Dominic M.Bowman

Instituut voorSterrenkunde, KULeuven

Low-FrequencyGravity Waves inMassive StarsRevealed by High-Precision K2 andTESS Photometry.

Almost all massive stars inevitably end their lives in a violentsupernova explosion and form a black hole or neutron star.Supernovae enrich the interstellar medium with chemicalelements and impact the next generation of star formation andthe evolution of their host galaxy. However the mass of thecompact remnant and the supernova chemical yield dependstrongly on the internal physical properties of the progenitorstar, which are currently not well-constrained fromobservations. The large theoretical uncertainties in the modelsof massive star interiors accumulate throughout stellarevolution, with the lack of a robust theory of stellar structureand evolution being particularly pertinent for evolved massivestars such as blue supergiants. Asteroseismology of stellaroscillations allows us to uniquely probe stellar interiors, yetinference from massive stars has been limited by a dearth ofdetected pulsations in such stars until recent space photometrymissions. In this talk, I report on the diverse pulsationalvariability discovered in a large sample of massive starsobserved by the K2 and TESS space missions. The discoveryof coherent pulsation modes and stochastic low-frequencygravity waves in numerous blue supergiants allow the interiorproperties of massive stars to be mapped from the mainsequence to the later stages of their evolution. Asteroseismicmodelling provides important constraints on ages, coremasses, interior mixing, rotation and angular momentumtransport, which are essential input parameters in stellarevolution models. The discovery of pulsational variability inspace photometry of blue supergiants provides a necessaryfirst step towards a data-driven empirical calibration oftheoretical evolution models for the some of most massiveand short-lived stars in the Universe.

DerekBuzasi

Florida Gulf CoastUniversity

Light Curves forAsteroseismologyfrom Full-FrameImages

The 30-minute cadence full-frame images collected by TESSduring the nominal mission provide an invaluable resource forscience ranging from stellar astrophysics to exoplanets.Drawing on the Kepler experience, the TESS AsteroseismicScience Consortium (TASC) has formed a collaborative effortto use TESS data for asteroseismology, and established aTESS Asteroseismic Science Operations Center (TASOC) to

produce light curves from full-frame images. In this talk, wewill present the TASOC pipeline for producing light curvesfrom full-frame images, including light curve extraction fromthe FFIs, light curve correction for instrumental effects,automated stellar variability classification, and verification ofabsolute time for the resulting photometry. We will describethe TASOC FFI data releases for the first TESS sectors whichinclude millions of light curves down to Tmag<15, andpresent comparisons of TASOC FFI light curves to othercommunity-driven efforts such as image-subtraction and theeleanor pipeline. Finally, we will highlight a broad range ofasteroseismic detections across the HR diagram enabled byFFI light curves.

TheronCarmichael

Harvard University Using TESS toUnderstand theBrown DwarfPopulation

Brown dwarfs are defined as objects with masses between 13and 80 times the mass of Jupiter. These limits are somewhatarbitrarily chosen to be the mass at which deuterium fusiontakes place ( ) and the mass at which hydrogen fusiontakes place ( ). Though motivated by physicalprocesses, these mass limits—particularly the lower masslimit—do not provide much insight on the formationmechanisms of the objects at these masses. To betterunderstand brown dwarf formation mechanisms, we look tothe brown dwarfs that orbit main sequence stars to examinetheir physical and orbital properties. Brown dwarfs that transitstars are quite rare with only 19 published and so we seek tofind more like these with the transit method. Given the natureof the internal pressure support mechanisms of brown dwarfs(electron degeneracy pressure), we expect them to be betweenat least the size of Saturn and Jupiter, but they may be evenmore inflated if they are younger than a few million years.This means that for most main sequence stars and even starsthat are slightly evolved, the transit depths produced bybrown dwarfs will be well within the sensitivity of thepremier transit survey mission for the next decade: the TESSmission. Additionally, because it is fully sensitive to short-period brown dwarfs that transit bright stars during itsprimary mission, TESS is well-suited to characterizing aparameter space of the brown dwarf population that has veryfew known objects. Transit light curves allow us to calculate abrown dwarf’s radius while we rely on follow up spectra andradial velocity measurements of the host star to determine abrown dwarf’s mass. These spectra also allow us to derive themetallicity and effective temperature of the star while asequence of radial velocity measurements reveal theeccentricity of the brown dwarf orbit. Together, the mass,radius, and orbital eccentricity of a brown dwarf holdvaluable information in testing substellar evolutionary modelsand help us understand how the evolution of a brown dwarfmight be different when it orbits a star. Ultimately, thesemodels help connect the evolution of a brown dwarf to how itformed, so, as we study this population, we should reconsiderthe arbitrary mass limits used to define brown dwarfs andbase them instead on their formation histories. In thispresentation, we report the detection and characterization of abrown dwarf from TESS Cycle 1 and we discuss itsimportance to the population of transiting brown dwarfs. Thisbrown dwarf, along with a few others discovered by K2, fallsin the middle of the driest part of the so-called “brown dwarf

desert”. We show where substellar evolutionary models agreeand disagree with observations of brown dwarfs and discusssome possible explanations why.

AshleyChontos

Institute forAstronomy,University of Hawaii

ExoplanetsOrbitingAsteroseismicTESS Stars

Individual studies of exoplanets orbiting asteroseismic starshave allowed for some of the most precisely characterizedsystems currently known to date. In addition, ensemblestudies have yielded unprecedented insights into proposedmechanisms for planet formation and evolution. TheTransiting Exoplanet Survey Satellite (TESS) is expected todouble the number of planets found around asteroseismicstars, thus providing stronger constraints for physicalprocesses that occur in planetary systems. Here we present thediscovery of TOI 197.01, the first transiting planet identifiedby TESS for which asteroseismology is possible. Combiningasteroseismology with transit and radial velocity observations,we show that the bright ( mag) subgiant is orbited bya hot Saturn every 14.3 days. With a planet density measuredto better than , TOI 197.01 is one of the bestcharacterized Saturn-sized planets to date, demonstrating thepower of TESS to characterize exoplanets and their host starsusing asteroseismology. Furthermore, we present additionalplanet candidates from the first systematic search ofasteroseismic TESS host stars from sectors 1-9.

AgnieszkaCieplak NASA GSFC

PhotometricLightcurveSignatures of BlackHoles and NeutronStars with MainSequence StellarCompanions

Gravitational microlensing, paired with Doppler Beaming andEllipsoidal Variations, is a new method of detecting blackholes (BHs) and neutron stars (NSs) in binaries with mainsequence stars. The TESS dataset with its precise photometryis especially well-suited to search for these self-lensingbinaries (SLBs). I describe our search for these SLBs usingTESS and present our model for these lightcurve signaturesused to fit potential BH/NS candidates. I present possibleexamples of lightcurves with some of these signatures foundthrough our search in the TESS dataset.

RyanCloutier University of Toronto

Present and FutureEfforts for the PRVCharacterization ofSouthern TESSPlanets Throughthe HARPS Mdwarf Program

The hi-resolution HARPS spectrograph has been operating atthe ESO 3.6-m telescope in La Silla, Chile for nearly twodecades. In that time, HARPS has consistently achieved sub-m/s radial velocity precision that makes it particularly well-suited to the characterization of sub-Neptune-sized planets inthe southern sky. On behalf of members of the on-goingHARPS M dwarf program, I will present results obtained thusfar into TESS's lifetime which includes the precisecharacterization of a number of warm terrestrial planetsrepresenting some of the closest transiting M dwarf planetarysystems to the solar system. I will also discuss future plans toexpand our program by obtaining simultaneous near-IR radialvelocities using the NIRPS spectrograph starting in 2020. Anupgrade that will further solidify HARPS + NIRPS asdominant instruments for the precise characterization ofplanet masses around nearby small stars.

KarenCollins

CfA/SAO TFOP SG1Ground-basedTime-seriesPhotometry: Goals,Status, Results andYour TESS Paper

The TESS Follow-up Observing Program Working Group(TFOP WG) is a mission-led effort organized to efficientlyprovide follow-up observations to confirm candidates asplanets or reject them as false positives. The TFOP WG isorganized as five Sub Groups (SGs). This talk discussesTFOP SG1, the ground-based time-series photometry SubGroup. TESS has 21 arcsec pixels and photometric apertureswith radius ~1 arcmin, which are often contaminated with

many stars. The primary goals of the SG1 team are todetermine the source of a TESS detection and/or identifyphotometric false positives prior to conducting observationswith more precious follow-up resources that produce high-resolution imaging and precise radial velocities. SG1observations also improve the precision of TESSephemerides, confirm the accuracy of TESS deblended transitdepths, and/or provide transit time variation (TTV)measurements. For planet validation efforts, SG1 observationsoften constrain the source of the TESS detection to within asmall follow-up photometric aperture, and measure transitdepths in multiple filter bands to place limits on chromaticity.In addition to describing the TFOP SG1 goals, strategy, andcurrent status, I will discuss how to access, interpret, andmake use of TFOP SG1 data in your TESS paper.

IanCrossfield MIT

Spitzer Transits andEclipses of TESSPlanets

Soon JWST will launch and become the world-leadingfacility in the atmospheric characterization of transitingexoplanets. One of the key goals of TESS is to provide JWSTwith the best exoplanet targets for detailed characterization. Iwill report on our ongoing Spitzer program to measure precisetransits and eclipses of the most interesting TESS planets foratmospheric study. Early results include secondary eclipses ofseveral planets with a range of sizes, precise transit timing,and IR radii for many new systems. This program is settingthe stage for HST and JWST spectroscopy of some of TESS'smost intriguing new discoveries.

Jason Curtis Columbia University Searching forYoung Exoplanetsin DispersedClusters Guided byGyrochronology

Knowing stellar ages is essential in this era of precisionastrophysics. Our current inability to provide confident agesfor stars negatively impacts the development of theories forplanet formation and evolution. The K2 mission alleviatedthis by targeting star clusters and associations, with planetsdiscovered in Upper Sco (10 Myr), Praesepe (670 Myr), theHyades (730 Myr), NGC 6811 (1 Gyr), and Ruprecht 147 (2.6Gyr). Unfortunately, the Pleiades (130 Myr) was exhaustivelysearched and no exoplanets were found. Clusters might thenseem to be ideal targets for TESS; however, their oftencrowded environments combined with TESS's large pixelsmakes this difficult in most cases. Fortunately, Gaia offers analternative route: a variety of spatially dispersed groupings ofstars are found in DR2 including nearby stellar streams, tidaltails associated with clusters (e.g., Hyades, Praesepe, ComaBer), and known and new young moving groups. Each bringsnew prospects for finding young planets in benchmarkablesystems by virtue of their spatially dispersed positionscompared to dense cluster cores, which mitigates thecrowding challenge. We validate candidate members for thesevarious systems by comparing the rotation periods wemeasure from TESS light curves to the cluster perioddistributions inherited from the Kepler/K2 era (i.e., ensemblegyrochronology). For example, we confirm the existence ofthe Hyades tidal tail observed during Cycle 1 by showing thatits stars follow the same rotation period distribution as thecluster core. Regarding the cluster-planet age gap betweenUpper Sco and Praesepe, consider Pisces-Eridanus (Psc-Eri),a nearby (d = 80-226 pc) stellar stream stretching across 120degrees of the sky, which was recently discovered with Gaiaby Meingast et al. (2019). We measured rotation periods forover 100 members observed so far by TESS and found that it

has a rotation period distribution nearly indistinguishablefrom that of the Pleiades, indicating that they are coeval. Thismakes the Psc-Eri stream an exciting source of young starsand exoplanets located in a more diffuse environment that isdistinct from that of the Pleiades and of other dense starclusters. Indeed, we determined that HD 1160 is a memberand host to a directly imaged object near the hydrogenburning limit, and we already discovered a multi-planetsystem transiting a G dwarf member with TESS. Ourcharacterization of Psc-Eri is the first gyrochronology studyusing TESS data, and it confirms that TESS will be anexciting mission for stellar astrophysics. This is especiallytrue given how TESS records and releases FFI data. Theexistence of this stream was not known prior to the TESSCycle 1 call for proposals, and yet the FFI data were ready forus to analyze immediately following the stream's discovery.

DrakeDeming Univ. of Maryland

A Bayesian Look atthe PlanetOccurrence Ratefrom TESS

Although TESS is not a statistical mission, the TESS data areamenable to statistical analyses using Bayesian techniques.We are engaged in a two-phase analysis of the planetoccurrence rate in TESS data. First, we use occurrence ratesfrom Kepler, as well as other astrophysical information, aspriors to estimate the prevalence of false-positives and realplanets among the TESS candidates. As the validation processby the TESS team becomes more complete, our analysis willenter a second phase wherein we derive TESS occurrencerates independently, and compare to Kepler and the ground-based surveys.

NardielloDomenico

Universita degli Studidi Padova (Italy)

PATHOS: a PSF-based Approach toTESS High QualityData Of StellarClusters

The TESS mission will observe about of the sky in twoyears giving us the possibility to search for new variable starsand exoplanets in many Galactic fields. During the mission ahuge sample of dense stellar systems (open and globularclusters and young associations) will be observed in FullFrame Images mode and 30-minute cadence. The mostdifficult challenge is the extraction of high-precisionphotometry of stars located in such crowded environments. Inthis context, we took advantage of our expertise gained byworking with HST and Kepler data to develop a PSF-basedmethod for the extraction of high-precision light curves fromTESS images. This innovative technique, mainly based on theuse of empirical PSFs and high-angular resolution inputcatalogs (like Gaia DR2), allows us to subtract neighborsources to a target star and measure its real flux minimizingthe contamination due to the neighbors. In this way we canobtain high-precision photometry for stars located in crowdedfields or too faint (T>14) to be measured using simpleaperture photometry. The project PATHOS is mainly focusedon finding exoplanet candidates in stellar clusters. Moreover,our work shall be intended as preparatory for the high-precision photometry and light curve extraction on data fromfuture space-based missions, such as PLATO.

DianaDragomir

MIT The HD 21749System: ATemperate Sub-Neptune and theFirst Earth-SizedPlanet Discoveredwith TESS

I will present the discovery of an exoplanet system thathighlights the state-of-the-art capabilities of TESS in thecontext of both time coverage and photometric precision. HD21749 is a K4.5 dwarf star located just 16 pc away from theSun, and is newly known to host two small transiting planets.Planet b is an unusually dense sub-Neptune in a 35.6-dayorbit, with a radius of and mass of . It

was possible to measure this planet's period in large partthanks to the four-sector TESS time series for this star. Planetc orbits the star with a period of 7.8 days and measures

, demonstrating that TESS can easily detect Earth-and sub-Earth-sized planets around bright stars. It isnoteworthy that (in addition to the TESS data) this discoverywas made possible almost entirely by existing ground-basedspectroscopic and photometric observations that weregenerously contributed by several teams. Since the HD21749system is a prime target for comparative studies of planetarycomposition and architecture in multi-planet systems, I willdiscuss a few exciting follow-up avenues that are currently, orwill soon be, within reach.

Nora Eisner University of Oxford

Planet HuntersTESS: People-Powered ExoplanetDiscovery in TESSData

I will present new results from the Planet Hunters TESSproject, which exploits the power of citizen science to findtransit events in the TESS data by engaging tens of thousandsof volunteers. While most planets in the transit survey datawill be found using purpose-built algorithms and software,some are unavoidably missed – in particular if the signals aresomehow unusual. Results from the Kepler version of PlanetHunters showed that humans can outperform the automateddetection pipelines for certain types of transits, especiallysingle (long-period) transits, as well as aperiodic transits(circumbinary planets) and planets around rapidly rotating,active stars (young systems). I will discuss the benefits andchallenges of using citizen science to find transit signals; howwe make use of the vast numbers of user classifications; andhow we evaluate the sensitivity of our planet search usingsimulated transit signals. I will also briefly outline the role ofdiscussion forums, moderators, and researcher feedback inensuring a positive user experience, as well as in highlightinginteresting systems quickly. Finally, I will provide anoverview of the planet candidates that we have found so far.

ZahraEssack

MassachusettsInstitute ofTechnology (MIT)

Low AlbedoSurfaces of LavaWorlds.

Hot super Earths are exoplanets with short orbital periods (<10 days) whose rocky surfaces reach temperatures highenough to become molten. There are a few hot super Earthsthat exhibit high geometric albedo values (> 0.4) in the Keplerband (420-900 nm). Sources of reflected light that maycontribute to the high albedos include: Rayleigh scattering inan atmosphere that may contain visible wavelength absorbers,reflective clouds, and/or the planetary surface. In this study,we focus on reflection from planetary surfaces. We aim todetermine whether specular reflection from molten lava andquenched glass (a product of rapidly cooled lava) on thesurfaces of hot super Earths may be a source of reflected lightthat contributes to the high geometric albedos. Weexperimentally measure the specular reflection from roughand smooth textured quenched glass, and survey non-crystalline solids literature for specular reflectance valuesfrom molten silicates as a proxy for specular reflectancevalues for lava. Integrating the empirical glass reflectancefunction and non-crystalline solids reflectance values over thedayside surface of the planet at secondary eclipse yields anupper limit for the albedo of a lava-quenched glass planetsurface of . We conclude that lava planets with solid(quenched glass) or liquid (lava) surfaces have low specularalbedos, and hence a negligible contribution to the geometricalbedos of hot super Earths. Literature values for diffuse

reflectance from planetary glasses also result in low planetaryalbedos. TESS has discovered 11 hot super Earth candidatesthat are awaiting follow-up observations and futurecharacterization as potential lava worlds.

MichaelFausnaugh MIT

Type IaSupernovaeObserved in theFirst Six Sectors ofTESS Data.

I will present early time light curves of 18 Type Ia supernovaeobserved in the first six sectors of TESS data. For eight ofthese objects with sufficient dynamic range (greater than 3.0mag from detection to peak), I will detail results fromcharacterizations of the initial explosion and searches forsignatures of companion stars. Most of the supernovae areconsistent with fireball models where the flux increases as ,while two sources display a flatter rise with flux proportionalto t. There is no obvious evidence for additional structuresuch as multiple power law components in the early risinglight curves. Assuming a favorable viewing angle, one canplace conservative upper limits on the radii of any companionstars of less than for six supernovae and less than for 4 supernovae. If such systems are commonplace, the oddsof non-detection in this sample are for companionsgreather than and for companions greater than

. At the current rate, TESS will either detect emissionfrom a dwarf companion during its initial two year survey, orplace stringent limits on single-degenerate progenitor models.I will also provide an update on this analysis for additionalbright supernovae found in the first year of TESSobservations.

AdinaFeinstein University of Chicago The Eleanor

Pipeline

During its two year prime mission the Transiting ExoplanetSurvey Satellite (TESS) will perform a time-seriesphotometric survey covering over of the sky. This surveycomprises observations of 26 24x96 degree sectors that areeach monitored continuously for approximately 27 days. Themain goal of TESS is to find transiting planets around200,000 pre-selected stars for which fixed aperturephotometry is recorded every two minutes. However, TESS isalso recording and delivering Full-Frame Images (FFIs) ofeach detector at a 30 minute cadence. We have developed anopen-source software, eleanor, will provide light curves for 26million sources in the TESS Input Catalog brighter than I=16throughout the Southern Hemisphere. eleanor is also availablefor users to generate their own light curves. I will describe themethods used in eleanor to produce light curves that areoptimized for planet searches. The tool performs abackground subtraction, aperture and PSF photometry,decorrelation of instrument systematics, and cotrending usingprincipal component analysis. I will specifically discuss themost recent improvements to these methods and the next stepswe plan on taking to maximize the photometric capabilities ofthe TESS FFIs.

JulianaGarcia-Mejia

CfA | Harvard-Smithsonian

The TierrasObservatory: AnUltra-PrecisePhotometer toCharacterizeNearby TerrestrialExoplanets

We are currently building the Tierras Observatory, a 1.3multra-precise fully-automated photometric observatory locatedatop Mt. Hopkins, Arizona dedicated to following up nearbytransiting planets discovered by TESS and other surveys,refine estimates of their radii, and find the longer period (andhence more temperate) worlds. Tierras will regularly achievea photometric precision of 700 ppm, enough to measure thetransit of planets orbiting stars with 3σsignificance. I will provide an overview of the current state of

the observatory, as well as the design choices that will enableits science goals. These include: (i) a custom designed four-lens focal reducer and field-flattener to increase the field-of-view (FOV) of the telescope from a 12" to a 0.5 degreediagonal; (ii) a 4K 4K pixels deep-depletion low read noiseCCD operated in fast frame transfer (shutterless) mode with

quantum efficiency at the wavelength of observation(compared to for regular CCDs); (iii) a custom narrow(50 nm) bandpass filter centered at 865 nm to minimizeprecipitable water vapor errors, known to limit ground-basedphotometry of red dwarfs; and (iv) a custom-made nano-fabricated beam-shaping diffuser (Stefansson et al., 2017) tomold the focal plane image star into a broad and stable top-hatshape, increasing the dynamic range of our observations whileminimizing flat-fielding, guiding, and phase-induced errorsdue to seeing. Tierras will be on-sky by January of 2020, intime to carry out plenty of follow-up observations of TESStargets in the northern hemisphere. This work is supported bythe National Science Foundation, the Ford Foundation, theJohn Templeton Foundation, and the Harvard Origins of LifeInitiative.

MaximilianGuenther MIT

Stellar Flares andHabitable(?) M-dwarf Worlds:Exploring a NewSample with TESS

Finding and characterizing small exoplanets orbiting M-dwarfs naturally poses the question of exoplanet habitability.A major contributing factor to this might be stellar flares,powerful magnetic reconnection events on the star. Flares canerode or sterilize exoplanets’ atmospheres and completelydiminish their habitability - but they might also be required totrigger the genesis of life around M-dwarfs in the first place.Here, I will highlight our study of stellar flares from theTransiting Exoplanet Survey Satellite (TESS). In the first fewmonths alone, we already identified hundreds of flaring M-dwarfs, superflares with up to 30x brightness increase, andbolometric flare energies ranging from to erg. I willlink our results to criteria for prebiotic chemistry, atmosphericloss through coronal mass ejections, and ozone sterilization.Ultimately, stellar flare studies will aid in defining criteria forexoplanet habitability for the many temperate worlds TESS isset to discover.

NataliaGuerrero

MIT TESS ScienceOffice

TESS Objects ofInterest Catalog:Sectors 1-6

The Transiting Exoplanet Survey Satellite (TESS) observedsix partially overlapping sectors in the ecliptic SouthernHemisphere from July 2018 to January 2019, as part of itsmission to observe of the entire sky in two years andmeasure masses for 50 planets less than . Each sectorcovers of the sky and the partially overlapping sectors1-6 cover of the sky. We describe the process to createthe TESS Objects of Interest (TOI) catalog from Sectors 1-6.The catalog consists primarily of planet candidates andknown planets. The TESS Follow-Up Observing Program(TFOP) has prioritized and observed TOIs using theExoplanet Follow-up Observing Program (ExoFOP) tocoordinate effort and share data. The TESS data products forsectors 1-6, including the TESS Object of Interest catalog,light curves, full-frame images, and target pixel files, aremade available to the public on the Mikulski Archive forSpace Telescopes (MAST).

Zhao Guo Pennsylvania StateUniversity

The Variability ofTESS Eclipsing

We search for eclipsing binaries with variabilities and deepeclipses in TESS 2-min cadence data. We distinguish between

Binaries variabilities from stellar activities such as spots and thosefrom pulsations. Specifically, we focus on the upper-mainsequence pulsators in eclipsing binaries, including the F- andA-type Gamma Dor and Delta Scuti stars and the SlowlyPulsating B-stars and Beta Cephei stars. We also identifysystems with high eccentrics and possible tidally excitedoscillations. A list of promising targets is compiled forfollow-up observations

JJ Hermes Boston UniversityFirst Light onPulsating CompactObjects with TESS

The vast majority of both isolated and binary stars, as well asnearly all known planet hosts, will end their lives as whitedwarfs. There are thousands of compact remnants locatednear enough to Earth that they are bright enough for usefulTESS observations, and hundreds of these objects vary onshort (minutes to hours) timescales that can be fullycharacterized by one month of TESS data. I will present somefirst-light analysis and results from the active working groupon compact pulsators within the TESS Asteroseismic ScienceConsortium, including precision insight into the corecomposition of a stellar remnant, as well as what we canexpect from continued TESS observations.

Klaus WHodapp

University of Hawaii,IfA

The EXor OutburstLightcurve of ESO-Ha 99

The process of accreting mass onto a forming young starsusually proceeds at an accretion rate that is insufficient toaccumulate a typical stellar mass in the time commonlythought to be available for this process. However, thisrelatively quiescent state of low accretion occasionally getspunctuated by much more intense accretion events thatmanifest themselves as photometric outbursts and that may beresponsible to much of the final mass of a star. Gaia alert18dvz first noted a substantial rise in brightness of youngstellar object ESO-H_alpha 99 embedded in the dense high-extinction cloud Sandqvist~1, which is seen against theRCW~27 HII region in Vela. ATLAS archival data allowed totrace the light curve back several years and indicate a prior,but minor flux maximum. Optical (Faulkes Telescope) andinfrared spectroscopy (IRTF) show prominent emission lines,the characteristics of an EX Lupi (EXor) outburst event.Based on UKIRT and IRIS data, ESO-H_alpha 99 isassociated with a reflection nebula and one molecularhydrogen emission knot, indicating past jet activity. TESS hascovered ESO_Halpha 99 in sector 8 of its southernhemisphere survey and gave a detailed light curve with atemporal resolution of an hour. This light curve covers anintermediate dip in brightness a few weeks prior to reachingthe brightness maximum of ESO-H_alpha 99 and showsunprecedented detail of the temporal evolution of theaccretion luminosity with flickering down to timescales ofhours.

MattHolman

Harvard CfA A TESS Search forDistant Planets

Several lines of evidence, both theoretical and observational,indicate that additional planets in the outer solar systemremain to be discovered. We recently developed a noveltechnique to search for solar system bodies (Holman et al.2018). This method is particularly well-suited to very slow-moving objects, even those for which the motion within a daymight be to small to detect. We present the results of our useof this method to search for distant planets and minor planetsin existing TESS data. Perhaps even more important than thesearch itself is a detailed, quantitative analysis of the survey's

detection limits and biases. This information is essential forthe rigorous interpretation of these survey results. Suchsimulators have been developed for CFEPS/OSSOS,NEOWISE, and other surveys, leading to detailed results onthe small body populations throughout the solar system. Wehave developed a high-fidelity survey simulator for Pan-STARRS and have extended it to TESS. This simulator takespositions, magnitudes, and rates of motion calculated from asolar system model (Grav et al 2011) at the times andlocations of individual exposures. It then inserts syntheticdetections into the resulting exposure source catalogs,accounting for the details of the camera, photometric zeropoint, and other essential details. The source catalogs,including synthetic detections, are then run through our fullsearch pipeline. This approach allows a clear, quantitativestatement about the prevalence of distant planets, as seen byTESS.

ThomasHoloien

CarnegieObservatories

ASASSN-19bt:The First TDEDetected by TESS

In January of 2019, the All-Sky Automated Survey forSupernovae (ASAS-SN) discovered a tidal disruption event(TDE) in the TESS Continuous Viewing Zone. The TESSlight curve provides unprecedented high-cadence monitoringof the TDE host and the rise of the transient's light curve,allowing us to precisely constrain the time of first light andthe rise time, which has never been done before with a TDE.In my talk I will discuss our full dataset, including the TESSlight curve, and how the TESS data have allowed us to gainnew insights into the physics behind TDE emission.

ChelseaHuang

MassachusettsInstitute ofTechnology

Planets from theTESS Full FrameImages

The TESS Full Frame Images provide a unique opportunityfor a magnitude limited sample of planetary candidates. Usingthe Quick look pipeline, we performed photometric extractionand planet detection on the first 9 sectors of TESS Full FrameImage data. We then selected the planetary candidates using aconvolutional neural network based machine learningtechnique (astronet-tess). We report the planetary candidatesdetected in stars with Tmag<11, and a preliminary estimationof the detection completeness rate of the pipeline. We willtake a first look into the planet population around these brightstars. We will discuss the comparison between the actual yieldfrom our pipeline compare and the pre-launch planet yieldsimulation, and the implications about planet populations.

DanielHuber

University of Hawaii Asteroseismologyof Solar-Type Starswith TESS

Asteroseismology is a unique observational tool to probe theinteriors of stars, and a benchmark method to determinesurface gravities, masses, radii and ages of solar-type stars.TESS enables the powerful extension of asteroseismology tobright stars with independent observational constraints,allowing the systematic investigation of poorly understoodphysical processes in stellar models such as convective energytransport and mode excitation for hot solar-type stars. In thistalk I will present first results from TESS 2-minute cadenceobservations of solar-type stars allocated to the TESSAsteroseismic Science Consortium (TASC), including anoverview of the target selection, an evaluation of the currentphotometric performance of TESS for asteroseismic studies,and the discovery of oscillations in high-profile targets suchas the metal-poor benchmark star nu Indi. I will conclude withan outlook on the expected total yield of asteroseismicdetections in the nominal TESS mission, and prospects for

asteroseismology of solar-type stars with a potential extendedmission.

Kate Isaak ESA

CHEOPS:CHaracterisingExOPlanet Satellite– a missionoverview

CHEOPS (CHaracterising ExOPlanet Satellite) is the firstexoplanet mission dedicated to the search for transits ofexoplanets by means of ultrahigh precision photometry ofbright stars already known to host planets. The first S- orsmall-class mission in ESA’s Cosmic Vision 2015-2025, themission is a partnership between Switzerland and ESA, withimportant contributions from 10 other member states. It willprovide the unique capability of determining accurate radii fora subset of those planets in the super- Earth to Neptune massrange, for which the mass has already been estimated fromground- based spectroscopic surveys. It will also provideprecision radii for new planets discovered by the nextgeneration of ground- and space-based transit surveys. Bycombining known masses with CHEOPS sizes, it will bepossible to determine accurate densities of subsaturn sizeplanets, providing key insight into their composition andinternal structure. By identifying transiting exoplanets withhigh potential for in-depth characterisation – for example,those that are potentially rocky and have thin atmospheres -CHEOPS will also provide prime targets for futureinstruments suited to the spectroscopic characterisation ofexoplanetary atmospheres. The high photometric precision ofCHEOPS will be achieved using a photometer covering the

waveband, designed around a single frame-transfer CCD which is mounted in the focal plane of a 30 cmequivalent aperture diameter, f/5 on-axis Ritchey-Chretientelescope. CHEOPS will reach a photometric precision of 20parts per million in a 6 hour observation of a v-bandmagnitude 9, G-type ( K) dwarf, commensuratewith measuring the transit depth of an Earth-size planettransiting the same star to a signal-to-noise of 5. In the case offainter stars, CHEOPS will reach a photometric precision of85 parts per million in a 3 hour observation of a v-bandmagnitude 12, K-type ( K) dwarf. CHEOPS willlaunch in the timeframe of October-November 2019. ofthe observing time in the 3.5 year nominal mission lifetimewill be taken by the Guaranteed Time Programme, defined bythe CHEOPS Science Team. The remaining will beavailable to Guest Observers from the Community through acompetitive proposal submission process, comprising annualCalls and a discretionary time component. In this presentationI give an overview of the mission, including scienceobjectives, capabilities and expected performances and theopportunities to use CHEOPS.

Jon M.Jenkins

NASA AmesResearch Center

TESS ScienceProcessingOperations CenterPipeline and DataProducts

TESS launched 18 April 2018 to conduct a two-year, near all-sky survey for at least 50 of Earth’s nearest neighboringexoplanets for which masses can be ascertained and whoseatmospheres can be characterized by ground- and space-basedfollow-on observations. TESS just completed its survey of thesouthern hemisphere, identifying hundreds of candidateexoplanet systems and unveiling a plethora of exciting non-exoplanet astrophysics results, such as asteroseismology,asteroids, and supernova. The TESS Science ProcessingOperations Center (SPOC) at NASA Ames Research Centerprocesses the image data downlinked from TESS every two

weeks to generate a range of data products hosted on theMikulski Archive for Space Telescopes (MAST). The SPOCscience pipeline is modeled on that of NASA’s historic KeplerMission. For each sector (~ one month) of observations, theSPOC calibrates the image data for both 30-min Full FrameImages (FFIs) and up to 20,000 pre-selected 2-min target starpostage stamps. A number of time series data products aregenerated for the 2-min targets, including simple aperturephotometry and systematic error-corrected flux time series.The SPOC also conducts searches for transiting exoplanets inthe 2-min data for each sector and generates Data Validationtime series and associated full, one-page summary, and mini-reports for each transit-like feature identified in the search.The accumulated data-to-date in each hemisphere are alsosearched for exoplanets to discover longer period planetstransiting stars observed over multiple sectors, includingthose in the James Webb Continuous Viewing Zone (CVZ),which are observed for up to one year. The data products alsoinclude co-trending basis vectors (CBVs) and calibration files,such as the Pixel Response Function (PRF) across the field ofview of each of TESS’s four cameras. To maximize the easewith which the community can use them, the TESS sciencedata products are modeled after those for Kepler and includeTarget Pixel Files (TPFs) containing original and calibrated 2-min image data, Light Curve files (LCs) containing thephotometric time series for each 2-min target, as well as theData Validation products. In this talk, I describe the SPOCpipeline, the pipeline products, and the chief differencesbetween the TESS and the Kepler pipelines, and the majorupdates to the SPOC pipeline (4.0) available now to thecommunity at MAST. I also discuss the documentationavailable to the community to help them in properlyinterpreting and analyzing the TESS data products. The TESSMission is funded by NASA’s Science Mission Directorate asan Astrophysics Explorer Mission.

JamesJenkins Universidad de Chile

TESS Discovery ofthe First Ultra-HotNeptune

In this talk I will discuss our HARPS radial-velocity follow-up observations of candidates detected by TESS, thosereleased as TESS Objects of Interest (TOI) to the communitythrough the TESS Alerts system. In particular, I will focus onthe planet candidate orbiting the star LTT9779 (TOI-193),which is a bright (V=9.8 magnitudes), super metal-rich, andSun-like star. The planet falls in the Neptune desert, yet it hasan orbital period of only 19hrs, making it the first such planetever detected. I will briefly discuss the nature of the system,possibilities for formation and evolution mechanisms for theplanet, and how LTT9779b can be a useful laboratory to studythe atmospheric physics and chemistry of extreme superNeptunes. Finally, I will give a brief overview of other TOIsthat we have observed as part of our HARPS precision radial-velocity follow-up program, discussing other systems wehave confirmed and our ongoing efforts in the southernhemisphere.

ColeJohnston

KU Leuven Coupling BinarityandAsteroseismology:High-PrecisionCore Masses and

For decades, eclipsing binary systems have been heralded fortheir ability to provide high-precision constraints on stellarmodelling. Indeed with their ability to prove model-independent (dynamical) masses and radii, eclipsing binarysystems have long served as calibrators for distances, ages,and theoretical models of stellar structure and evolution. As

Ages from Keplerand TESS

such, eclipsing binaries are often used in studies to investigatethe poorly understood processes of chemical and angularmomentum transport in stellar interiors, particularly forintermediate- to high-mass stars born with convective cores.The most glaring difference between theory and observationsis the so-called mass discrepancy between evolutionary anddynamical masses. This mass discrepancy is often solved byincreasing the core mass in stellar evolution models byintroducing additional near-core boundary mixing viarotation, overshooting or penetration, or any combinationthereof in stellar models. These phenomena each have thepotential to increase the core mass of the star. However, thereis much debate as to what the proper implementation andscaling of such mechanisms should be. In this talk, we reviewthe results of using binaries to constrain such interior mixingprocesses and their effect on the resulting core masses andages. We discuss the phenomena of rotation, overshooting,penetration and internal gravity waves as mechanisms toinduce interior chemical mixing and angular momentumtransport, as well how binary modelling can criticallyconstrain such processes. We also showcase the potential ofcombining contemporary binary and gravity-modeasteroseismic modelling to provide independent crossconstraints for the calibration of interior transport processes.Finally, we point out how binary asteroseismology based onspace-based photometry, in combination with updatedastrometric solutions from future Gaia releases can lead toprecise predictions of He-core masses and ages at the end ofthe main-sequence.

StephenKane

University ofCalifornia, Riverside

TESS Observationsof KnownExoplanetarySystems

At the current time, it remains unknown if many of the radialvelocity detected exoplanets transit their host stars. Sincethese host stars are relatively bright, they provide numerousopportunities for detailed characterization of the systems,such as transmission spectroscopy, orbital dynamics, andpotential targets for future imaging missions. Our TESS Cycle1 Guest Investigation conducted high cadence observations ofthe southern exoplanet host stars, including known transitingplanets, and combined these photometry with updatedplanetary orbits from radial velocity analyses. Our programhas searched for transits and phase variations for thesesystems, refined transit ephemerides, and collaborated withnumerous other teams who are using our TESS Cycle 1program to characterize known exoplanetary systems. In thispresentation we provide a summary of TESS science achievedthus far for the known exoplanets, including new results ontransit searches, detection of phase variations, and refinementof planetary orbits, particularly for systems observed by TESSover multiple sectors. We provide details for both Cycle 1 and2 statistics regarding overall expectations for TESS detectionsin known systems and how these discoveries contribute to theoverall TESS yield in terms of exoplanet demographics.

ElizaKempton

University ofMaryland

How to DetermineWhether M-DwarfTerrestrial PlanetsPossessAtmospheres

The promise of the TESS mission is that it will detect legionsof planets for which atmospheric characterization will bepossible with JWST. Perhaps the most exciting among theseplanets are the rocky ones, which up until now have not beenaccessible to atmospheric studies. Yet small rocky planets willstill be challenging targets for JWST, so the question arises ofhow best to use JWST to make tangible progress toward

understanding the atmospheres of terrestrial bodies. We positthat JWST is best suited to distinguish between rocky planetsthat do and do not possess atmospheres by photometricallyobserving the secondary eclipses of these objects. Theargument is as follows. The day side temperature of a tidallylocked planet will always be reduced by the presence of anatmosphere, either because the atmosphere transports heat tothe night side of the planet or because atmospheric scattererssuch as clouds will increase the planet’s Bond albedo. Thereis therefore a maximal secondary eclipse depth that isrepresentative of a hot dayside hemisphere with noatmosphere present. We focus on planets orbiting M starsbecause these are the ones that will be discovered in largenumbers by the TESS mission, they are within theobservational grasp of JWST, and there is considerableskepticism as to whether these planets can retain atmospheresat all given the high-energy irradiation environment aroundtheir host stars. I will present the results from a multi-institution collaboration investigating the promise and thelimits of secondary eclipse photometry as a test for candidateatmospheres on rocky M-dwarf planets. We have developed asuite of general circulation models (GCMs) and radiative-convective atmospheric structure models, and have developedour understanding of rocky planet surface geochemistry, inorder to address this topic. We have focused our efforts onthree warm transiting super-Earths that will be ideal targetsfor secondary eclipse investigations with JWST — GJ 1132b,TRAPPIST-1b, and LHS 3844b. The final planet on this list isa TESS-discovered super-Earth that is likely representative ofa larger number of such objects that will be discovered overthe remainder of the mission. Finally, we have quantified themodest amount of JWST observing time that is required todistinguish between planets with and without atmospheresusing secondary eclipse photometry. This will be comparedagainst the time required to perform the same test using phasecurves and the more traditional transit spectroscopytechniques. Being able to do so is important, because it willallow us to make the most efficient use of JWST's limitedresources in the exploration of rocky exoplanet atmospheres.

LauraKreidberg Harvard University

The Thermal PhaseCurve of LHS3844b

TESS is rapidly discovering the best planets in the sky fordetailed atmosphere characterization. One of these newdiscoveries is LHS 3844b, a terrestrial planet in an 11-hourorbit around a nearby M-dwarf. We recently measured athermal phase curve of LHS 3844b with the Spitzer SpaceTelescope. In this talk, I will present the data and discussconstraints on the planet’s atmospheric properties based onthe observed phase variation.

David W.Latham

Center forAstrophysics |Harvard &Smithsonian

Masses and Radiiof Exoplanets fromKepler, K2, andTESS

The population of planets orbiting solar-type stars isdominated by planets smaller than 4 Earth radii, the size ofNeptune. Mass determinations for transiting planets identifiedby Kepler and K2 have suggested that most planets smallerthan about 1.8 Earth radii have bulk densities that areconsistent with internal structures and compositions similar tothe terrestrial planets in the Solar system. One of the primarygoals of the TESS mission is to determine masses and bulkdensities for more than 50 planets smaller than , toimprove our understanding of the transition between rocky

planets and those more like Neptune. We will show theprogress towards this goal.

ElisabethMatthews MIT

High-ResolutionFollow-Up ofTESS CandidatePlanets with 8m-Class Telescopes

I will report on our large-scale program of high-resolutionimaging of TESS candidates with 8m class telescopes. Thiseffort is essential in order to check for blended stars whichcan (at best) dilute the TESS light curves and bias themeasured planet radii of the observed planet, or (at worst)indicate an astrophysical false positives. I will present initialresults from our diffraction-limited optical+infrared imagingusing Gemini and VLT, which are sensitive to stellarcompanions at just a few 10s of milliarcseconds. Our datahave already identified blended companions to several TOIs,while verifying that most TOIs are free from contaminationby nearby stars. I will also describe our work combining ourhigh-resolution imaging with GAIA data to measure themultiplicity of TESS planet hosts across a range of planetaryand stellar properties.

AmberMedina

Center forAstrophysics |Harvard andSmithsonain

Flare Statistics andHigh ResolutionSpectroscopy of aVolume CompleteSample of Mid-to-Late M dwarfswithin 15 Parsecs

Main-sequence stars with masses less than that of theSun are fully convective and are the most abundant stars inthe galaxy. The question of how fully convective starsgenerate their magnetic field is of intrinsic interest and alsobears upon the habitability of their orbiting planets. We arecurrently undertaking a multi-epoch high-resolutionspectroscopic survey in addition to obtaining (through a TESSGI program) two-minute cadence data of a volume-completesample of stars with masses between 0.1-0.3 the solar valueand within 15 parsecs. The stars in the sample are wellcharacterized with accurate masses and radii, and photometricrotation periods from the MEarth project. We will determinethe statistics of flares on all mid-to-late M dwarfs within 15parsecs. We will use our complementary high-resolutionspectroscopic measurements of rotational velocities, equivalent widths, along with our galactic space motions(calculated from our measured radial velocities) to correlatethe ages and activity levels of this population to the flarerates, luminosities, and durations.

Kristo Ment Harvard University Uniting TESS Dataand a Decade ofGround-BasedObservations bythe MEarth Project

For 11 years, the ground-based MEarth survey has beenmonitoring nearby M dwarfs in pursuit of transiting Earth-likeplanets. The MEarth target sample has a significant overlapwith the TESS Candidate Target List. This provides a uniqueopportunity to complement high-precision TESS photometrywith the long temporal base line of MEarth data. TESS hasalready provided high-quality photometric data for the twoMEarth-discovered terrestrial planets orbiting LHS 1140(Dittmann+ 2017, Ment+ 2019). Conversely, MEarth datahelped to independently confirm the ultra-short-period TESSplanet around LHS 3844 (Vanderspek+ 2018) anddemonstrated that the star was inactive and spinning with along rotation period of 128 days. We are currentlyundertaking an extensive phase-folded search of theaccumulated MEarth data to identify new planets, and confirmor rule out TESS planet candidates. Combining MEarth andTESS data paves the way for assembling the first-evervolume-complete list of transiting planets within the habitablezones of nearby mid-to-late M dwarfs. This work has beensupported by the National Science Foundation, the David and

Lucile Packard Foundation, and the John TempletonFoundation.

TravisMetcalfe

Space ScienceInstitute

Disentangling theRotation andActivity Variationsof 94 Aqr fromAsteroseismologywith TESS

Previous efforts to calibrate how rotation and magneticactivity depend on stellar age and mass have relied onobservations of clusters, where stellar evolution models areused to determine the properties of the ensemble.Asteroseismology employs the same models to measure theproperties of an individual star by matching its normal modesof oscillation, yielding the stellar age and mass with muchhigher precision. We use 27 days of photometry from theTransiting Exoplanet Survey Satellite (TESS) to characterizethe solar-like oscillations of a G8 subgiant in the 94 Aqr triplesystem. The resulting stellar properties, along with areanalysis of 35 years of activity measurements from theMount Wilson HK project, allow us to disentangle therotation and activity variations observed in the system. Thederived age agrees with gyrochronology for the cool dwarfs inthe system, but the rotation period of the subgiant is muchshorter than expected from standard models of angularmomentum evolution. I will discuss these results in thecontext of recent evidence that gyrochronology is less usefulfor stars beyond the middle of their main-sequence lifetimes,and outline how asteroseismic calibration of an empiricalactivity-age relation could provide reliable ages for starsbeyond middle-age.

MarcoMontalto Universita di Padova

Mining TESS FullFrame Images(FFIs) to Analyzethe Brightest Dwarfand Sub-GiantStars of the Sky.

The TESS satellite is revolutionizing the field of time domainastronomy since, for the first time, an unbiased sample ofnearly all sky sources can be studied with unprecedentedphotometric precision. While boosting our knowledge onexoplanetary systems, the lightcurves extracted from TESSdata will also represent an important legacy upon whichforthcoming characterization (e.g. CHEOPS, JWST, ARIEL)and planet hunting missions (e.g. PLATO) will base theirfuture target selection strategies. In this talk I will focus onthe analysis of a broad sample of carefully selected FGKMdwarf and sub-giant stars monitored by TESS during its firstyear of observations. I will present a customized pipeline aptto mine TESS FFIs, extract optimized, homogeneous, multi-sector photometry and search for transiting planets. Finally, Iwill discuss the planet candidate yield and statistics as well asthe on-going efforts to promote follow-up analysis.

BenjaminMontet University of Chicago

Turning PlanetCandidates intoPlanets in the TESSFull-Frame Images

While considerable attention has been given to those targetstargeted at two-minute cadence in the TESS mission, the vastmajority of planet candidates are expected to be found in theTESS Full-Frame Images. With one million stars observed persector, these images provide an opportunity to understandplanet occurrence in different stellar environments, aroundstars of different masses and ages. However, this dataset alsoprovides unique challenges for finding, characterizing, andvalidating planet candidates. I will provide an update onplanet candidates detected through the eleanor pipeline forlight curve extraction from the TESS Full-Frame Images andstrategies for turning these candidate transit signals into bonafide planets with TESS data, including our strategies toincorporate machine learning into planet validation.

ElisabethNewton

Dartmouth College DS Tuc Ab: A 45Myr Old Planet in

We present the first results from the TESS Hunt for Youngand Maturing Exoplanets (THYME) Project: the discovery of

the Tuc-Hor YoungMoving Group

DS Tuc Ab, a transiting planet in the 45 Myr Tucana-Horologium young moving group. We first identified transitsusing photometry from the Transiting Exoplanet SurveySatellite (TESS; the candidate was alerted as TIC 200.01).The host star, DS Tuc, is a visual binary and is unresolved inthese data; we use our follow-up observations to demonstratethat the transit signal derives from the primary component,DS Tuc A (HD 222259A, G6V). Using a suite of new andarchival data, we improved the stellar parameters andvalidated the planet. We find no additional stellar or planetarysignals in the data. We highlight two unusual properties of theplanetary system. First, the close-in planet is larger thanNeptune but smaller than Saturn ( ), falling in asparsely populated region of the radius--period diagram.Second, the host star's spin axis, the planet's orbital axis, andthe visual binary's orbital axis are likely aligned to within 10degrees.

BelindaNicholson

University ofSouthern Queensland

Single TransitFollow up withMinerva-Australis

Single transit events represent planets that are in temperateenvironments on longer orbits, and are thus far a poorlysampled area of parameter space of exoplanet systemarchitectures. We present the radial velocity measurementsfrom the University of Southern Queensland's Minerva-Australis facility for a selection of single transit planetcandidates from TESS. Using these radial velocity measurewe are able to confirm these planet candidate, constraining theorbital periods and estimating the planet masses. These alsoprovide interesting candidates for follow up studies such asatmospheric characterisation and system architectures.

Louise D.Nielsen Geneva Observatory

TOI-125: PreciseMassDetermination ofThree Level-1TESS Planets

We present intensive HARPS radial velocity follow-up of thetransiting multi-planet system TOI-125 (TIC 52368076)validated by Quinn et al. 2019. TOI-125 is a bright, , K0 dwarf star, which hosts three mini-Neptunes detected inTESS Sector 1 and 2 data. TOI-125b has an orbital period of4.65 days, a radius of , a mass of

, yielding a mean density of g cm .With an orbital period of 9.15 days, TOI-125c is near the 1:2mean motion resonance with its inner companion. It has asimilar radius of and a mass of ,implying a mean density of g cm . The outer transitingplanet, TOI-125d, has an orbital period of 19.98 days. With aradius of , mass , it is denserthan the two inner planets ( g cm ). Our jointanalysis of the RVs and TESS light curves also providesupper mass limits for the two low-SNR planet candidatesreported by Quinn et al. 2019; TOI-125.04 ( ), anultra-short period super-Earth with a period of 0.53 days, andTOI-125.05, a planet with an estimated radius of

possibly sitting between TOI-125c and TOI-125d at 13.28 days. We cannot confirm the presence of TOI-125.04, for which we find a mass upper limit of 1 Me. We findno evidence of TOI-125.05 in our RVs, and estimate a massupper-limit of , which excludes it as a viable candidate inthe system. We discuss the internal structure of the threeconfirmed planets, as well as possible formation and evolutionscenarios with and without the two additional candidates,which cannot be confirmed with our present data.

Ryan Vanderbilt University Differenced Our team has released high-precision, difference imaging

Oelkers Images, LightCurves, andVariability Metricsfor All StarsObserved in TESSFull Frame Images

light curves, differenced images, TESS Input Catalog stellarparameters, Lomb-Scargle periodicity information, Box-Least-Squares eclipse information, and basic variabilitymetrics for more than 50 millions stars observed in TESS full-frame-images. We released these data products, through theFiltergraph visualization portal at the URLhttps://filtergraph.com/tess_ffi, providing users a uniqueopportunity to interact with the data. Filtergraph allows itsusers to quickly plot light curves, visualize stellar parameters,and investigate trends in a single portal. These data productshave been shown to be as precise as official NASA dataproducts, and have already led to independent communitydiscoveries. I will provide a brief description of the reduction,and a short tutorial of the public data release on Filtergraph.

Dr HughOsborn

Laboratoired'Astrophysique deMarseille

RapidClassification ofTESS PlanetCandidates withConvolutionalNeural Networks

As space-based survey missions such as TESS provide moreand more planet candidates, accurately and rapidly classifyingtransiting exoplanets from photometry is a goal of growingimportance. Here I present results from on-goingcollaboration between machine learning and astronomicalresearchers to perform this work using neural networks. Thisincludes results as obtained on real Kepler planet candidatesfrom DR24 ( average precision, Ansdell et al 2018), andresults from 4 sectors of high-fidelity, pixel-level TESSsimulations data ( average precision, Osborn et al 2019).I will also present the first application of a neural-networkbased classifier to real TESS data, from which we recover

of TOIs coincident with candidates, and propose afurther 200 TCEs as planet candidates for which follow-up isongoing.

James Owen Imperial CollegeLondon

Testing thePhotoevaporationModel with TESSMultis

Photoevaporation of natal H/He envelopes is one of theleading theories to explain the radius gap observed to separateclose-in, super-Earth and sub-Neptunes sized planets.However, without measurements of planetary masses andwith planet radius data alone, testing the photoevaporationmodel is difficult. Fortunately, TESS will provide a largesample of planets for which radial velocity follow-up toconstrain their masses is possible. I will describe the uniquepower of multi-planet systems that contain both super-Earthand sub-Neptune sized planets in testing the photoevaporationmodel, wherein the photoevaporation model predictsminimum masses for planets in the system. The power ofmulti planet systems arises because one of the criticaluncertainties in testing the photoevaporation model is theXUV activity history of the star; however, in multi-planetsystems, one knows all planets orbit the same star andexperience the same XUV history. Given a multi-planetsystem with measured radii, I will demonstrate how thephotoevaporation model predicts the planet's minimummasses, which can then be tested with targeted radial velocityfollow-up. Kepler only provided a handful of systems forwhich this analysis can be done; however, TESS shouldprovide a large sample of systems to test the photoevaporationmodel qualitatively. As a demonstration, I will presentpredicted minimum masses for planets in the TOI-270 system.Finally, I will argue that consideration of photoevaporation'spredictions in selected systems for radial velocity follow-upcan maximise the scientific value of the data. This usefulnessis because photoevaporation's predictions are minimum

masses, so even a non-detection can still be used to refute thephotoevaporation model.

Andras Pal Konkoly Observatory TESS in the SolarSystem

Although TESS observes fields further away from the Eclipticin its primary mission, thousands of minor planets areobserved in each of these sectors that otherwise haveinclinations higher than a few degrees. In this presentation,we review the most essential aspects of Solar System studiesusing TESS as a photometer for the analysis of known minorbodies. Photometry of these objects are performed from anunusual perspective: the computation of apparent position aswell as the efficient selection of objects appearing in a certainfield-of-view also imply some non-trivial issues. Based on thelight curves of these asteroids, one could not only concludethe fundamental physical characteristics (such as rotationperiod and shape constraints) in an unbiased manner, butvariations on the longer timescales lead us to a deeperunderstating of surface properties. Regarding to the moresophisticated photometric processes, we present algorithms --along with the bottlenecks in the respective implementations -- which will allow us to see and characterize objects whichare fainter than the single-frame detection limit of the TESScameras. Since the main-belt asteroids form the mostprominent sample of such objects of the Solar System, it isimportant to investigate whether our observations are biasedor not in terms of the distribution of the proper orbitalelements. Therefore, we also summarize briefly how thevarious dynamical families are sampled in the primarymission due to the avoidance of the vicinity of the Ecliptic.Besides the aforementioned statistical analyses, someparticular objects are also displayed which exhibit prominentfeatures if one investigates the corresponding light curves indetails. One of these examples is the candidate for the largestand brightest tumbling asteroid, where this tumbling naturehas been revealed by such long, uninterrupted and well-sampled light curves which can now only be provided byTESS.

Enric PalleInstituto deAstrofisica deCanarias

A Planetary SystemAround the NearbyM Dwarf Gl 357

We report the detection of a transiting Earth-size planetaround Gl357, a nearby M2.5V star, using data from theTransiting Exoplanet Survey Satellite (TESS). The newlydiscovered planet Gl 357b (TOI-562.01) is a transiting hotEarth-like planet with a radius of and anorbital period of day. Precise stellar radial velocitiesfrom CARMENES as well as archival data from HIRES,UVES, and HARPS, also display a 3.93-day periodicity,confirming the existence of the planet and leading to planetarymass of . In addition to the radialvelocity signal for Gl 357b, a second periodicity with

day indicates the presence of a second, non-transiting planet candidate in the system, Gl 357c, with aminimum mass of . The star is relativelyinactive and exhibits a photometric rotation period of

days. Gl 357b is the second closest transitingplanet to the Sun; its brightness makes it a prime target forfurther investigations, such as atmospheric spectroscopy andis, to date, the best terrestrial transiting planet suitable foratmospheric characterisation with the upcoming JWST andthe ground-based ELTs.

Anna Payne Institute forAstronomy,University of Hawaii

The SpanishDancer Puts on aShow: The 2018Outburst of NGC1566.

In late June 2018, increased hard X-ray emission was detectedfrom NGC 1566. Soon after, UVOT data collected using theNeil Gehrels Swift Observatory showed a significantbrightening, in tandem with the ASAS-SN light curveshowing dramatic variability. Combining data taken usingTESS, Swift, ASAS-SN, and Las Cumbres Observatory, weanalyzed 4263 photometric observations spread out over ~100days following the flare. Swift's X-ray and UV/optical,ASAS-SN's g-band, and TESS's redder filter make an idealcombination for continuum reverberation mapping studiesbecause it provides broad wavelength coverage. We willdiscuss our measurements of inter-band correlation and lagused to ultimately test and constrain continuum-emission diskaccretion models. In the era of TESS, our goal is to performthis analysis on a large scale. By discovering and studyingvariable AGN with TESS in combination with othersincluding ASAS-SN, we will be able to create a robust sampleto investigate the cause of variability. This will ultimatelyshed light on the nature of black holes and their surroundinghigh-energy environment.

Geisa Ponte

Centro deRadioastronomia eAstrofisica Mackenzie(CRAAM) -UniversidadePresbiterianaMackenzie

PhotometricVariability andMagnetic Activityin Young Suns

We investigate the impact of the chromospheric activity onprecise 2 minute-cadence NASA/TESS lightcurves of aselected sample of young solar twins (with ages between 50to 500 Myr). These stars were also monitored by benchmarkplanet hunter ESO/HARPS spectrograph over the course of, atleast, one rotational period. We estimate photometricvariability of lightcurves due to rotational modulations andexplore its correlations with classical spectroscopic indicatorsof chromospheric activity (such as Ca II lines), ages androtational periods. This valuable dataset will help us tounderstand the implications of magnetic activity variability inexoplanetary searches and the concept of habitability. Thiswork is an integrant part of a larger effort aimed atcharacterizing comprehensively (photometrically andspectroscopically) the magnetic fields in young suns.

StefanieRaetz

Institute forAstronomy andAstrophysics (IAAT)Tuebingen

The Rotation-Activity Relationof M dwarfs: FromK2 to TESS andPLATO

Studies of the rotation-activity relation of late-type stars areessential to enhance our understanding of stellar dynamos andangular momentum evolution. Photometric observations withspace telescopes such as the K2 and TESS missions providerotation periods even with low amplitudes as well as a wealthof activity diagnostics. We currently study the rotation-activity relation with K2 for M dwarfs where it is especiallypoorly understood. Our study is based on the Superblinkproper motion catalogue of bright and nearby Mdwarfs by Lepine and Gaidos (2011).The rotation-activityrelation based on photometric activity indicators revealed,that, at a critical rotation period of d, the activity levelchanges abruptly. This phenomenon represents an openproblem within the framework of dynamo theory. Despite theoutstanding capabilities of K2, the short observationalbaseline and the low cadence allows us to detect only shortrotation periods and long duration flares which represents astrong bias for such activity studies. TESS observes in its twoyears main mission almost all bright M-dwarfs from theSuperblink catalogue. Although TESS observes one sector foronly d, it will provide up to thirteen 27d-light curves for

of the targets due to the overlap of the sectors. TESSdrastically enlarges our sample of continuous high cadence

monitored bright M-dwarfs and allows us to study in depththe activity and in particular the morphology of flares. In thefuture, the PLATO mission with its unprecedented precision,short cadence and long observational baseline, allows us tostudy the magnetic activity indicators in up to now unrivaleddetail. In my talk I will explain the results of our K2 studyand show the application of the activity analysis methods toTESS data. Furthermore, I will describe how a higher cadenceand a longer duration improves the determination of rotationperiods and the detection of stellar flares.

GeorgeRicker MIT

The TESS Mission:History, PresentStatus, and FutureProspects

In this talk, a brief history will be related as to how and whythe TESS project came to be. The current status of themission will also be summarized. Finally, as we jointlycelebrate the exciting results from TESS in its initial year--aswell as the prospects for TESS in its first extended mission --an attempt will be made to foresee a few of the excitingpossible future discoveries that TESS may make in thecoming decade(s).

RyanRidden-Harper

Australian NationalUniversity

Discovering RapidTransients in theTESS BackgroundSurvey

TESS offers an exciting opportunity to search for new andexotic transients with lifetimes less than a day. Due to thatlarge field of view, TESS will serendipitously observe manytransients, that may go undiscovered. Through the TESS:Background Survey, we are able to systematically search allTESS TPFs and FFIs to provide the largest high cadencesurvey to date. I will discuss the TESS: Background Survey,and present the unique objects that were discovered in thesesurveys alongside new rates for short lived exotic transients.

JoeyRodriguez

Center forAstrophysics |Harvard &Smithsonian

Using TESS toUnderstand GiantPlanet Migration

Nearly a quarter century since the discovery of the first hotJupiters, we are still trying to understand their underlyingevolutionary mechanisms. The orbital eccentricities of hotJupiters hold clues to their formation and dynamicalevolution, but most of these planets reside on very closeorbits, which circularize quickly due to tidal interaction withthe host stars. Hot Jupiters with periods longer than about 5days experience weaker tidal forces and can retaineccentricity for many billions of years. We refer to thesesystems where the circularization timescale is longer than thesystem’s age as “dynamically young Jupiters”. Unfortunately,there are only a few of these planets known and fewer stillhave precise eccentricity measurements. NASA’s TESSmission is well-suited to discover these longer period hotJupiters since ground-based surveys struggle to obtain thephase coverage necessary for initial detection. Using the FullFrame Images (FFIs) from TESS combined with groundbased RV and photometric observations, we have alreadydiscovered and measured precise eccentricities for  3 Jupiterswith periods longer than 5 days. We are actively observinganother 6 candidates from both the FFIs and pre-selected 2minute cadence targets. I will present our recent discoveriesand discuss the current hot Jupiter population in the context ofevolutionary mechanisms. 

SurangkhanaRukdee

Harvard CollegeObservatory/PontificiaUniversidad Catolicade Chile

TARdYS: AnUpcomingExoplanet Hunterin SouthernHemisphere

The relatively close habitable zone to the host stars of thevery common cool-low mass stars makes M dwarfs attractivefor finding habitable planets. We developed TARdYS, aspectrograph for the observation of cool stars in the southernhemisphere, where few high-resolution near-infraredspectrographs are available. TARdYS is a dual fiber fed,

white pupil Echelle and with an image slicer can yieldR>50,000 in the Y band ( ). It will beinstalled at the Tokyo Atacama Observatory TAO 6.5 mtelescope. I will discuss the overall instrument system designand ongoing development of this upcoming exoplanet hunterin the southern hemisphere, and its capability forcharacterizing TESS exoplanets.

Sarah JaneSchmidt

Leibniz Institute forAstrophysics Potsdam(AIP)

Initial ResultsFrom the TESSUltracool DwarfSurvey

Ultracool dwarfs are a class of objects that include both thesmallest stars and the warmest brown dwarfs, spanningspectral types M7 and later. They are intrinsically variablesources due both to the properties of patchy clouds on theirsurfaces, and to magnetic activity that gives rise to surfacespots and dramatic flares. This magnetic activity is found onthe majority of ultracool dwarfs, because fast rotation periodsand strong magnetic fields persist to older ages than for mainsequence stars. We present initial stellar properties, rotationperiods, and flare frequency distributions for the brightest 77ultracool dwarfs (spanning spectral types M6-L3) observedwith TESS through Sector 8 as part of our two-minutecadence sample. We measure rotation periods for half thesedwarfs, spanning a few hours to a few days. We also use theflare finding code AltaiPony to identify 177 flares on 39targets, and present initial flare frequency distributions.

Lizhou Sha MIT

Does WASP-47 eHave a Friend?Refining theOccurrence Rate ofInner Companionsto Hot JupitersUsing TESS Full-Frame Image Data

To date, WASP-47 e remains the only known innercompanion to a hot Jupiter (Becker et al. 2015). This apparentscarcity is broadly in line with the hypothesis that most hotJupiters form beyond the ice line and move inwards via high-eccentricity migration (HEM). However, statistical evidencebased on the dearth of super-eccentric hot Jupiters in Keplerdata suggests that HEM does not explain the formation of allhot Jupiters, leaving the possibility for some hot Jupiters tohave close-in planets (Dawson et al. 2015). TESS brings agolden opportunity to study the occurrence rate of hot Jupitercompanions in terms of both quality and quantity: not onlydoes TESS have enough photometric precision to detectsuper-earths around bright stars, but its full-frame images willalso provide more than double the number of high-precisionlight curves for hot Jupiters compared to Kepler and K2combined. Using the first eight sectors of TESS full-frameimages, we generate light curves for confirmed andcandidate hot Jupiters brighter than the 11th TESS magnitudewith the MIT Quick Look Pipeline. Having carefully removedthe known planet signal, we perform a uniform BLS searchfor companions in order to derive a constraint on theoccurrence rate of such planets. Combining this constraintwith the ones derived from Kepler and K2 hot Jupiters, wearrive at a refined upper limit on the occurrence rate of innercompanions to hot Jupiters. We then discuss the implicationsof this newly calculated occurrence rate and how it informscurrent discussions on the formation theories of hot Jupiters.

Krista LynneSmith

KIPAC at SLAC,Stanford University

The TESS-FermiBlazars

I will present the first results of the multiwavelengthmonitoring program of four gamma-ray bright Fermi blazars.These beamed relativistic AGN jets have been monitored fora full year in the optical, UV, X-ray, and gamma rays byTESS, Swift, and Fermi. The cross-correlation analysis ofsuch light curves offers insight into the emitting regionswithin relativistic jets, and whether the physical origin of the

high-energy emission arises from hadronic or leptonicprocesses. I will also discuss the expansion of this project inTESS Cycle 2, which includes radio data.

Jamie TayarInstitute forAstronomy,University of Hawaii

Calibrating StellarModels in theTESS Era

Different grids of stellar models predict different temperaturesand luminosities for stars of the same mass and age. In thepast, these differences were much smaller than themeasurement uncertainties, and could therefore be ignored.However, in the era of TESS and Gaia, the systematicuncertainties resulting from the choice of stellar model gridcan now be significantly larger than the formal measurementuncertainties when inferring the masses and ages of planethost stars. I will show how these uncertainties vary as afunction of luminosity, temperature, and metallicity anddiscuss ways of accounting for this effect. While theseuncertainties are a problem for planet characterization, theyrepresent an opportunity for improving our understanding ofstellar evolution. I will therefore also show that asteroseismicmeasurements of TESS dwarfs and subgiants, as well aslegacy data from the Kepler mission, can be used to constrainstellar physics, including the effects of rotation andconvection, and discuss how these constraints will improvewith future TESS data.

JohannaTeske

CarnegieObservatories

The Magellan-TESS Survey

Recent results on the characterization of small planets havepresented two questions: (1) Do super-Earth () and sub-Neptune ( ) planets form the same ordifferently? and (2) What is the precise *and* accurate planetmass-radius relation in the < regime? In this talk I willdescribe the methodology behind the Magellan-TESS Survey,designed to address these questions in a statistically robust,open framework by measuring the masses, host starcompositions, and system architectures of small TESSplanets across a range of insolation fluxes. I will also shareresults thus far and lessons learned that may be applicable toanalogous programs in the Northern Hemisphere.

RolandVanderspek MIT

TESSObservations:Looking to Year 2

The first year of the TESS prime mission has been completed,and Year 2 observations of the northern ecliptic hemispherehave begun. Because of the orientation of the TESS orbit,with apogee in the southern ecliptic hemisphere, scatteredlight from the Earth and moon will play a more prominentrole in Year 2 observations. I will review the prospects forYear 2 observations, which include changes in spacecraftpointing in Sectors 14 and 15. In addition, I will touch ontweaks in spacecraft operations that will lead to better overallscientific performance.

StevenVillanuevaJr.

MITSearching forLong-PeriodPlanets in TESS

I will discuss the progress in confirming and characterizingTESS long-period (P ⪞ 20 days) planets, specifically thoseidentified as single-transit events (STE). I will discuss theefforts to identify and vet STEs, including an overview of ouridentification pipeline. STEs require more careful planningand lengthier follow-up campaigns for confirmation thanmultiply transiting or short-period planets, but can yield someof the longest-period planets that TESS can find. I will discusssome of the strategies and challenges specific to confirmingSTEs, and I will give an overview of the known STEs andgive an update on their status.

JenniferWinters

Center forAstrophysics |

Three Red Suns inthe Sky of the

The only terrestrial planets that will be spectroscopicallyaccessible in the near future will be those that orbit nearby

Harvard &Smithsonian

Nearest PlanetTransiting an MDwarf

mid-to-late M dwarfs. We present the discovery from TESSdata of LTT-1445Ab, a terrestrial planet transiting an M dwarfonly 6.9 parsecs away. Remarkably, the host stellar system iscomposed of three mid-to-late M dwarfs in a hierarchicalconfiguration which are blended in one TESS pixel. We usefollow-up observations from MEarth and the centroid offsetanalysis in the TESS data validation report to determine thatthe planet transits the primary star in the system. From high-resolution spectroscopy and imaging, we rule out the presenceof additional stellar or brown dwarf companions. We derive apreliminary orbit for the bound BC pair that reveals an edge-on and highly eccentric configuration. The planet has a radius1.4 times that of Earth, an orbital period of 5.4 days, and anequilibrium temperature of 428 K. With radial velocities fromHARPS, we place a three-sigma upper mass limit of

on the companion, confirming its planetarynature. The system is particularly favorable for ground-basedobservations to study the planetary atmosphere, as thecompanion stars provide a valuable calibration source withthe same spectral type as that of the primary star. This work issupported by grants from the National Science Foundationand the John Templeton Foundation.

RobWittenmyer

University ofSouthern Queensland

MINERVA-Australis: ASouthern TESSFollow-UpMachine

MINERVA-Australis at the University of SouthernQueensland's Mount Kent Observatory is the only southernhemisphere precise radial velocity facility wholly dedicated tofollow-up of TESS planets. Mass measurements of theseplanets are critically necessary to maximise the scientificimpact of the TESS mission, to understand the composition ofexoplanets and the transition between rocky and gaseousworlds. MINERVA-Australis is a partnership between MIT,UNSW Australia, George Mason University, University ofLouisville, Nanjing University, UC-Riverside, University ofTexas, and the University of Florida. The array is now fullyoperational, with five of the planned six 0.7m telescopes inplace. I give an overview and update of operations, and Ipresent our precise radial velocity results and orbital solutionsfor several TESS planets.

Ian Wong MIT Phase CurveStudies of KnownTransiting Systemswith TESS

In addition to the huge yield of new planets, TESS willprovide many science opportunities for known transitingsystems. Following the legacy of similar work carried outwith Kepler data, we seek to take advantage of thecontinuous, long-baseline photometry provided by the TESSmission to study phase curves. From a full-orbit phase curve,we can place constraints on such physical quantities as: (1)the planet's dayside temperature and Bond albedo, throughmeasurement of the secondary eclipse depth in the TESSband; (2) the efficiency of day-night recirculation of incidentstellar irradiation, via the amplitude and phase shift of theatmospheric brightness modulation across the orbit; and (3)the response of the host star to the gravitational interactionwith the orbiting planet, as expressed by the phase curvesignals due to Doppler boosting of the star's light and tidaldistortion of the stellar surface. As an exemplarydemonstration case, we recently published our analysis of thephase curve of WASP-18 from TESS Sectors 2 and 3(Shporer, Wong, et al. 2019), which reveals a strongsecondary eclipse signal and high signal-to-noise phase curvemodulations attributable to atmospheric brightness variation

and ellipsoidal distortion, as well as a weak but physicallyconsistent measurement of Doppler boosting. Since then, wehave expanded our efforts into a unified and systematic lightcurve analysis of all known transiting systems with predicteddetectable secondary eclipses and/or phase curve signals. Iwill present the latest results from this work and discuss themin the context of emergent trends in exoplanet atmosphericdynamics and comparisons with the predictions of theoreticalphase curve modeling.

Deb Woods LLAsteroid Detectionin TESS FullFrame Images

In the first year of operations, the Transiting ExoplanetSurvey Satellite (TESS) has delivered on its promise of highquality photometry of nearby stars for exoplanet discovery, aswell as provided valuable data for applications beyond itsmain mission. With a wide (96 24 deg2) field of view andpersistent coverage for the 27 day duration of each observingsector, the TESS full frame images (FFIs) offer a uniqueopportunity for the discovery and characterization of asteroidsin our solar system. Recognizing the substantial risk to Earthfrom asteroid impact, a Congressional directive to NASA wasissued in 2005, instructing NASA to detect, track, catalog,and characterize Near-Earth Objects (NEOs) of size 140meters in diameter or larger with a perihelion distance of lessthan 1.3 AU from the Sun. In support of these objectives, theNASA NEO Observations Program, within the PlanetaryDefense Coordination Office, has funded the development ofan asteroid detection pipeline to run on TESS data as part ofthe Lincoln Laboratory Near-Earth Asteroid Research(LINEAR) program. This presentation discusses themethodology of the TESS asteroid detection pipeline,including strategies for image normalization, tracking, andfalse alarm filtering. The strategies are helpful in pushing thedetection limit to fainter objects and reducing the impact fromthe crowded field. The resulting data set offers the opportunityfor executing asteroid population studies and building asteroidlight curves, as well as for supporting potential discovery ofNEOs.

Huiqin Yang NationalAstronomicalObservatories, CAS

The NewExpression onActivity--RotationRelation across H-R Diagram

We present a statistical study of flares based on the whole dataset of the Kepler mission, which could enable us to gauge theactivity--rotation relation from the view of flares. Wecalculate the flare activity of more than 3400 flaring starsfrom A-type to M-type. It is found that the activity--rotationrelation in the late-type star is clear—that is, a saturatedregime with a high activity level and an exponential decayregime with a low activity level corresponds to fast rotatorsand slow rotators, respectively. The slope of the unsaturatedregime is , which is consistent with previous studies.However, as we consider this relation across H-R diagram,one interesting fact is that the two regimes gradually becomedispersive as the temperature increases and the activity--rotation relation nearly disappears in the early-type stars.Combined with the Gyrochronology, we find that the mixingof stars of two different dynamos gives rise to the dispersion.We thereby propose a scenario on understanding the activity–rotation relation across the H-R diagram. Based on thescenario and the correspondence of dynamo with regard toactivity and rotation, we suggest a new expression on theactivity–rotation relation, in which the segmentation is on thebasis of the dynamo rather than the rotation period.

Xinyu Yao Lehigh UniversityPrecovery of TESSSingle Transitswith KELT

During the Transiting Exoplanet Survey Satellite (TESS)prime mission, 74% of the sky area will have an observationalbaseline of only 27 days. For planets with orbital periodslonger than 13.5 days, TESS can capture only one or twotransits, and the planet ephemerides will be difficult todetermine from TESS data alone. Follow-up observations oftransits of these candidates will require precise ephemerides.We explore the use of existing ground-based wide-fieldphotometric surveys to constrain the ephemerides of theTESS single-transit candidates, with a focus on theKilodegree Extremely Little Telescope (KELT) survey. Weinsert simulated TESS-detected single transits into KELTlight curves and evaluate how well their orbital periods can berecovered. We find that KELT photometry can be used toconfirm ephemerides with high accuracy for planets of Saturnsize or larger, with orbital periods as long as a year, andtherefore span a wide range of planet equilibriumtemperatures. We also demonstrate that by incorporatingsmall amounts of simulated RV follow up data, the recoveryrate can be increased significantly. The resulting ephemeridescan be used for follow-up observations to confirm candidatesas planets, eclipsing binaries, or other false positives, as wellas to conduct detailed transit observations with ground-basedor space-based facilities.

ZhuchangZhan MIT

ComplexRotationalModulation ofRapidly RotatingM Stars Observedwith TESS

We have searched for short periodicities in the light curves ofstars with Teff cooler than 4000 K made from 2-minutecadence data obtained in Transiting Exoplanet SurveySatellite sectors 1 and 2. Herein we report the discovery of 10rapidly rotating M dwarfs with highly structured rotationalmodulation patterns among 371 M dwarfs found to haverotation periods less than 1 day. Starspot models cannotexplain the highly structured periodic variations that typicallyexhibit between 10 and 40 Fourier harmonics. A similar set ofobjects was previously reported following K2 observations ofthe Upper Scorpius association. We examine the possibilitythat the unusual structured light curves could stem fromabsorption by charged dust particles that are trapped in or nearthe stellar magnetosphere. We also briefly explore thepossibilities that the sharp structured features in the lightcurves are produced by extinction by coronal gas, by beamingof the radiation emitted from the stellar surface, or byoccultations of spots by a dusty ring that surrounds the star.The last is perhaps the most promising of these scenarios.Most of the structured rotators display flaring activity, and weinvestigate changes in the modulation pattern following thelargest flares. As part of this study, we also report thediscovery of 17 rapidly rotating M dwarfs with rotationalperiods below 4 hr, of which the shortest period is 1.63 hr.Finally we report on the development of a variable starpipeline with machine learning applications and show otherinteresting objects the pipeline have discovered.

GeorgeZhou

CfA The Frequency ofHot Jupiters Acrossthe HR diagramfrom TESS

Nearly 25 years after the discovery of the first hot Jupiter,their formation is still not fully understood. These planets arefound in orbits of varying obliquities and eccentricities,orbiting stars ranging from M-dwarfs to A-stars, andreceiving incident fluxes ranging over 5 orders of magnitude.One way to unveil for their origins is to survey their

properties across a range of stellar environments. Theproperties of planets are intimately linked to the properties oftheir host stars, and TESS is uniquely positioned to explorethis link. We report the occurrence rate for hot Jupiters acrossthe main sequence, as measured via TESS FFI observations.TESS explores large sections of the sky, covering a widestellar distribution within the Solar neighbourhood. It is alsothe only survey that has the photometric precision to enable acomplete census of planets around stars as large as mainsequence A stars. We will present our frequency for hotJupiters from TESS, and compare them against that of Kepler,RV main sequence and evolved star surveys. Together, theseresults tell a tale of hot Jupiter evolution through space andtime.

Carl Ziegler University of TorontoOne Hit Wonders:Hunting for theLongest PeriodTESS Planets

TESS is looking at most of the sky for only 27 days during itsprime mission, and it is therefore not sensitive to most long-period transiting exoplanets. Around a thousand of theseplanets will transit once during the TESS observations manywith deep transits that would be detectable from the groundby a sub-meter aperture telescope. However, with largelyunconstrained ephemerides, these planets will be difficult tofollow-up and it is likely many will be unrecovered in theforeseeable future. The One Hit Wonders survey will hunt theNorthern single-transit planets using a robotic half-metertelescope. We use transit models to estimate the orbital periodfrom the TESS light curve and the stellar parameters, thenmonitor at long-cadence an ensemble of targets with expectedtransits each night. Images are reduced on-the-fly and thelight curves of each target are checked for possible transitswhich triggers a short-cadence, continuous observing mode.With a subsequent transit secured, the timing of future transitscan be determined and further observations outsourced toadditional telescopes to further confirm and characterize theplanet. We expect approximately twenty planets to berecovered in the first year. These discoveries will fill in acurrently sparse regime in the orbital period versus host starmagnitude parameter space. These planets will be excellenttargets for atmospheric characterization due to their brighthosts. These studies have primarily been performed on short-period planets in the past, in part due to a paucity of potentialtargets, and consequently little is known about theatmospheres of cooler planets.