Expected Yields of Planet discoveries from the TESS primary and extended missions
We present a prediction of the transiting exoplanet yield of the TESS primary mission, in order to guide follow-up observations and science projects utilizing TESS discoveries. Our new simulations differ from previous work by using (1) an updated photometric noise model that accounts for the nominal pointing jitter estimated through simulation prior to launch, (2) improved stellar parameters based on Gaia mission Data Release 2, (3) improved empirically-based simulation of multi-planet systems, (4) a realistic method of selecting targets for 2-minute exposures, and (5) a more realistic geometric distortion model to determine the sky region that falls on TESS CCDs. We also present simulations of the planet yield for three suggested observing strategies of the TESS extended mission. We report planets to be discovered by the TESS primary mission, as well as an additional planets for each year of the three extended mission scenarios we explored. We predict that in the primary mission, TESS will discover about 3500 planets with Neptune size and smaller, half of which will orbit stars with TESS magnitudes brighter than 12. Specifically, we proposed a new extended mission scenario that centers Camera 3 on the ecliptic pole (C3PO), which will yield more long period planets as well as moderately irradiated planets that orbit F, G, and K stars.
The successful launch of the Transiting Exoplanet Survey Satellite (TESS; Ricker et al., 2014, 2015) on 2018 April 18 marked the beginning of a new era for transiting exoplanet science. For the next two years, TESS will provide high precision time series photometric observations of bright stars across almost the entire sky. The TESS mission is designed to discover new planets orbiting bright stars spanning a wide range of spectral classes.
The brightness of the host stars will enable follow-up studies that can measure detailed properties of the planets. Coverage of a diverse stellar demographic will reveal previously unexplored planet populations. Moreover, with the timely second release of Gaia data (DR2) in April 2018 (Gaia Collaboration et al., 2016, 2018), the parent stars and the planets they host may be characterized better than ever before.
To exploit the scientific yield of the TESS mission, follow-up observations are expected to be a significant and essential part of the mission. Besides confirmation of the planetary nature of transit signals, follow-up studies will provide more complete characterizations of planetary systems, including, but not limited to, measurements of planet masses, orbital eccentricities, atmospheres (e.g., chemical composition, albedo, temperature, Seager & Deming, 2010; Crossfield & Kreidberg, 2017), and stellar obliquities (e.g., Gaudi & Winn, 2007; Albrecht et al., 2012). To date the majority of planets that have been characterized in detail with these methods are giant planets in close orbits around F, G, and K stars. TESS will provide the opportunity to answer questions such as: How diverse are the densities and compositions of close-in small planets? How diverse are the densities of planets formed in the same planetary system? How do planetary systems form around different types of stars? What are the properties of planets with irradiation intensities similar to that of the Earth? The Kepler mission has provided hints of the answers to some of these questions (e.g., Fulton et al., 2017; Weiss & Marcy, 2014; Weiss et al., 2018; Mulders et al., 2015). Given the expected improvement in the accuracy of planetary and stellar properties from TESS, we will be able to constrain some of these answers well enough to differentiate planet formation models.
A realistic estimation of TESS planet yields is expected to aid the efficient planning of follow-up observations, and to prepare the science community to use TESS results to address interesting scientific questions.
That is the subject of the work presented here. We carry out a simulation of TESS’s planet yield using our best knowledge regarding the mission observation plan, current understanding of exoplanet populations, and the stars that TESS will observe. The simulation is applied to the two-year primary mission, as well as three scenarios of the TESS extended mission (yet to be funded by NASA). We highlight the following components of our planet yield simulation that are intended to make it more accurate than previous work (i.e., Sullivan et al., 2015; Bouma et al., 2017; Barclay et al., 2018):
(1) Use of a photometric noise model that accounts for the nominal pointing jitter estimated through simulation prior to launch (Nguyen et al., 2018);
(3) A realistic process for selecting targets for the 2-minute cadence observations using the candidate target list (CTL; Stassun et al., 2017) and information from Gaia DR2, while keeping the number of targets per CCD to within the maximum allowed by the mission;
(5) Precise position and geometric distortion for the TESS field of view based on ray tracing results and pre-launch measurements.
We describe the simulation in detail in §2 and present the results for the TESS primary mission planet yield in §3. In §4 we describe three TESS extended mission scenarios, each lasting one or three years, and present the planet yield for each scenario. We conclude with a discussion and summary in §5.
2.1. TESS field of view and observing strategy
The TESS cameras, field of view, and observing strategy are described in detail in Ricker et al. (2014, 2015) and Sullivan et al. (2015). We give here a brief description including the details most relevant to the present planet yield simulation.
TESS consists of four identical cameras each with an entrance pupil diameter of 10.5 cm and a field of view (FOV) of (See Figure 1). The focal plane of each camera contains a mosaic of four 2058 pixel 2048 pixel CCDs with a pixel scale of per pixel. The four FOVs are positioned adjacent to each other, forming a total FOV of . The angular gaps between camera fields are 15 arcminutes, and within each camera the gaps between adjacent CCDs correspond to 35 arcminutes. These specific numbers describing a camera FOV are approximations used for convenience in the simulations.
During the primary mission the set of four fields is oriented along a line of ecliptic longitude from below the ecliptic equator to past the Southern ecliptic pole in TESS’s first year, and from above the ecliptic equator to past the Northern ecliptic pole in TESS’s second year. Therefore the field viewed by Camera 4 will be centered on either the Southern or Northern ecliptic pole, and fully contain the corresponding JWST continuous viewing zone (See Figure 1).
TESS is scheduled to start science observations of the first sector (Sector 1, or S1) in late June 2018 111TESS started its science observation on July 25, 2018.. In each of the first and second years, TESS will collect observations from 13 different sectors with a cadence of 27.4 days. Every TESS camera will take an exposure every 2 s. TESS will transmit to the ground mainly two types of data products made from the 2-s images by stacking. The first data product will consist of 2-min stacks from limited regions around preselected target stars (target pixels, TP). The second product will consist of full images from all the cameras stacked at a 30-min cadence. The planned TESS fields of view for the primary mission are illustrated in equatorial coordinates in Figure 2. We used the estimated mission pointing profile for the first year (Southern hemisphere) observations precomputed by the TESS team for the 18 April launch date and the nominal mission schedule 222Actual sector positions will depend on the start date of science operations.. The positions of the second year sectors are assumed to be symmetric about the ecliptic equator to the first year sector positions.
2.2. Star Catalogs
2.2.1 Target Pixel selection
The targets for 2-min cadence target pixels (TPs) were selected from stars in the Candidate Target List (CTL) (Stassun et al., 2017) with TESS-band magnitudes . We follow the mission requirement to limit the number of targets per CCD to 1,500, and the total targets per sector to 16,000. The target list is first populated with all the bright stars that fall on the science regions of the CCDs; then the list is reduced to satisfy the limitations on numbers by selecting targets from the CTL that have the highest priorities 333the priority is computed based on the suitability of detecting transiting planets around the target (see Stassun et al. (2017) for more details). When combing through the CTL we cross reference the star with Gaia DR2 parallaxes, if the star is indicated to be a giant in Gaia DR2, we do not include it in the 2 min cadence targets.
We note these particular constraints result in approximately half the number of 2-min targets in Camera 4 (pointing at the ecliptic pole, i.e., JWST continuous viewing zone), compared to what was assumed in Sullivan et al. (2015) and Bouma et al. (2017).
The preliminary TP list includes a total of 98,965 and 106,250 unique targets planned to be observed with 2-min cadence in the first and second year of operation, respectively.
2.2.2 Full Frame Images
We selected 2.6 stars in TIC-6 (Stassun et al., 2017) with catalog to be included in our Full Frame Image (FFI) simulation. The expected centroid locations of these target stars on the CCDs were predicted using a geometric model derived from prelaunch optical ray trace results (Woods et al., 2016). Only stars that fall on science pixels are considered. For stars with 12, we use the information from Gaia DR2 (Andrae et al., 2018) to update the TIC-6 stellar parameters. The match between Gaia DR2 and TIC-6 catalog listings is based on a cross match using ecliptic coordinates444The matching accounts for proper motion based on Gaia DR2 (epoch 2015.5, equinox J2000)., limiting the allowed difference between the Gaia () and TESS () magnitudes, as well as limiting the allowed difference between corresponding estimated values of . A more thorough incorporation of the Gaia DR2 catalog into the CTL and TIC is an ongoing task of the TESS Target Selection Working Group, and is beyond the scope of this paper. The typical uncertainty on the stellar radius from Gaia DR2 for our sample is 10%, which is comparable to the typical uncertainties from high-resolution optical spectra (combined with evolutionary models) obtained using Keck/HIRES for the Kepler planet host star sample (Petigura et al., 2017).
The Gaia DR2 stellar parameter estimation module imposes a lower limit on the stellar radius of 0.5 , which means the stellar radii from Gaia DR2 are not suitable for a large fraction of the M dwarf population. Therefore, for stars with TIC below 4,000 K we used the Gaia DR2 parallax to determine if the star is an M dwarf or an evolved giant star by estimating the stellar radius using the target’s distance and observed brightness. We then re-estimate the radius and mass of the M dwarfs following empirically calibrated model-independent relations between and radius (Mann et al., 2015).
Figure. 3 shows the distribution of stars observed by TESS in the HR diagram. Compared with Kepler, TESS will survey stars with a much broader spectral type distribution, hopefully detecting the planets of host stars spread throughout most of the HR diagram.
2.3. Planet Yield simulations
Our estimation of the planet population follows that of Sullivan et al. (2015). We adopted a planet occurrence rate for M dwarfs ( and ) per Dressing & Charbonneau (2015); for other stars, we adopted a planet occurrence rate per Fressin et al. (2013). For large planets, in the largest radius bin of Fressin et al. (2013), 6–22 , we re-sampled the radius within the bin boundaries from a Gaussian distribution centered on 1 , with a width of 0.2 .
The signal to noise ratio of the transit signal of a planet in a single TESS sector is calculated using:
in which, is the number of transits per sector, the transit depth , is the transit duration in hours between the second and third contact points, is the contribution of flux from neighboring stars relative to the total flux of the target star measured in the photometric aperture. For M dwarfs, we estimate the noise contribution from stellar variability over a 1-hour timescale by drawing from a log uniform distribution in the range 20-500 ppm. This is motivated by Figure 7 in Sullivan et al. (2015). For other stars, we assume , since their astrophysical variability amplitudes are typically smaller than the noise floor of TESS. We use the updated photometric precision estimates of Nguyen et al. (2018) for the expected TESS noise level over a 1-hour timescale . Similar to Sullivan et al. (2015), Nguyen et al. (2018) created synthetic images using model TESS point spread functions (PSFs) for different field angles 555In total, photometric noise is modeled as a function of at 5 different field angles in the simulation.. In addition, Nguyen et al. (2018) incorporated in the simulation the effect of spacecraft pointing jitter estimated on the basis of a prelaunch TESS fine pointing simulation. The overall noise performance is comparable to Sullivan et al. (2015) Figure 14, except that the systematic noise floor from jitter is around 40 ppm (rather than 60 ppm) for the bright stars ( 7), and slightly higher for the fainter stars. For each star, we first estimate the location of the star on TESS CCDs for each observation sector separately, and then adopt the noise model corresponding to the relevant portion of the detector. For targets observed in more than a single sector, we quadratically combine the signal-to-noise of the target from each observed sector to calculate the final signal-to-noise ratio (SNR) at a given time. We require a detected planet to have a SNR greater than 7.3 and at least two transits recorded by TESS.
2.3.1 Multiple planets
Our experience with the Kepler mission and ground based radial velocity surveys (Wright et al., 2009) has taught us that multi-planet transiting systems are abundant (Latham et al., 2011; Lissauer et al., 2011; Fabrycky et al., 2014; Tremaine & Dong, 2012). When accounting for multiplicity, previous studies typically simulate planets in the same system with independent occurrence probabilities, and assume the system to be perfectly co-planar (Sullivan et al., 2015; Bouma et al., 2017; Barclay et al., 2018). However, studies of Kepler planetary systems have revealed that there likely are correlations between the mutual inclination distributions and the true planetary multiplicities (Johansen et al., 2012; Hansen & Murray, 2013; Ballard & Johnson, 2016; Zhu et al., 2018). To more realistically investigate the multi-transiting planet systems that may be discovered by TESS, multiple planetary systems are injected into our simulations based on updated information on the dependence of a system’s mutual inclination distribution on the number of planets hosted by the target star. For stars other than M dwarfs, we follow the approach of Zhu et al. (2018) when the first planet in the system is not a hot Jupiter (a hot Jupiter is defined here as and day)666Since the companion occurrence rate in hot Jupiter systems is not well constrained.. The probability of a target star hosting a planetary system is 30%, while the probability of a star hosting planets ( 1–6) is evenly distributed777This is an approximation to the fitting result of the probabilities for each intrinsic multiplicity category fitted in Zhu et al. (2018). The systems hosting higher multiplicity are more likely to be co-planar, with the mutual inclination dispersion following a Rayleigh distribution in which the Rayleigh width is . For intrinsic single planet systems, the orientation of the planet’s orbit is selected at random.
For M dwarfs, we follow the simpler “Kepler dichotomy” approach of Ballard (2018). The probability of a target star hosting a single planetary system is 85%. For multiple planetary systems, we used the best fit value for Kepler M-dwarf systems from Ballard & Johnson (2016), with the average number of planets being , and the Rayleigh width of the mutual inclination distribution being . With a relatively small mutual inclination dispersion, the transit probability of a second planet is enhanced compared to the co-planar assumption, given the inner planet also transits. Ballard (2018) reported an enhanced planet yield by adding the mutual inclination distribution to the M-dwarf samples of Sullivan et al. (2015). We require that the multiple planetary systems follow the Deck et al. (2013) stability criterion: .
|FFI M888The FFI planet injection simulation is done independently from the TP injection simulation.||96||695||2260|
3.1. Primary Mission
Table 1 presents the yield of planets from the TESS primary mission. For the unique stars on target pixels, we expect to detect 2000 planets. The FFIs are expected to provide another detected planets. We show the sky positions of the detected planets in Figure 4. Stars with a higher number of detected transiting planets are mostly located close to the ecliptic pole, where the observational baseline for an average star is the longest. Figure 5 shows the distribution of periods and radii of the planets detected in the target pixels and the FFIs. Specifically, we examined the expected yields of planets from the target pixels after 4 and after 13 sectors of observation. More than 50 Level 1 999The Level One Science Requirement for the TESS Mission is to measure masses for 50 transiting planets smaller than 4 Earth radii planets () are expected to be detected in the first four science sectors101010The first TESS public data release will be the first four science sectors. As the data from each new sector accumulates, TESS will deliver smaller planets with longer orbital periods.
Figure 6 shows the number of planets TESS is expected to discover in the primary mission in different size categories. The majority of the smallest planets () from TESS discoveries will have both target pixel and FFI observations. This will ensure a more accurate determination of the transit ephemerides, and benefit follow up observations. Among the TESS discoveries, 1000 planets will be around stars with 10, which allows detailed characterization of planet properties using ground based facilities. The uncertainties on the planet yield estimation comes mainly from three sources: (1) Poisson statistical variations; (2) uncertainties in occurrence rates and our multiplicity model; and (3) the uncertainties in the stellar radii, especially for the late M dwarfs. Our planet yield estimate is comparable to previous works (Sullivan et al., 2015; Bouma et al., 2017; Barclay et al., 2018). Sullivan et al. (2015) used stars from galactic models, their yields are similar to our sample, especially for planets smaller than . We report a smaller number of discovered giant planets. This is because the Sullivan et al. (2015) FFI sample included stars slightly fainter than and TESS is able to discover giant planets beyond the magnitude limit in our simulation. Bouma et al. (2017) and Barclay et al. (2018) only simulated relatively bright stars: the yields from their simulations are between our mag and mag sample yields, as expected. We also compared our planet yields for M dwarfs with Muirhead et al. (2018). Their 50,000 brightest stars scenario is similar to a scenario with a magnitude limit of for M dwarfs. We predict planets from this sample, which is about 1.4 times higher. This enhancement in total number of planets is mostly due to our different assumptions relative to the occurrence rates of multiple planetary systems (see Ballard 2018).
TESS will also discover a few hundred systems in which a single star hosts multiple transiting planets. For the primary mission, we expect of the planetary candidates to be in multiple transiting planetary systems. For M dwarfs specifically, of the discovered system will have multiple transiting planets, consistent with the estimate of Ballard (2018).
We show the architecture of all predicted multiple transiting planet systems with 12, with known planets for comparison, in Figure 8. Though relatively few are known at present, TESS will identify hundreds of new multiple transiting systems around bright stars. Some of these systems will enable follow up observations to measure individual planet densities, atmospheres, obliquities, and eccentricities within the same system, leading to a better understanding of planet formation and evolution.
We expect that TESS will observe, during the primary mission, just one transit event for each of hundreds of longer-period transiting planets (Villanueava et al., 2018). We conservatively use a higher detection threshold for these events (SNR 10), and find that 75 and 689 of the single-transit events will be caused by true planets in the target pixels and FFIs, respectively. If they can be confirmed, these single-transit planets will uniquely expand certain exoplanet research avenues and even open new ones. These planets will extend the period range over which it will be possible to study the atmospheres and mass-radius relation of exoplanets, especially for FGK stars. If all the single-transit planets that are temperately irradiated (; Kopparapu et al. 2013) and have FGK dwarf star hosts can be confirmed, the number of such temperate planets will grow from 5 (that are expected to transit more than once in TESS light curves) to 16. Finally, while we did not explicitly include circumbinary planets (CBPs) in our yield simulations (so we do not have absolute numbers for their yield), we expect that the number of single-transit CBPs will be larger than the number of CBPs that TESS would otherwise find by at least a factor of a few (Quarles et al., 2018).
4. Extended Mission
4.1. Extended mission pointing scenarios
We investigated the following three pointing scenarios for the third year of TESS operations. The first two scenarios were also described in Bouma et al. (2017), for which we re-evaluate the outcomes with our updated simulations. We did not evaluate the Pole scenario from Bouma et al. (2017) because that scenario brings one of the camera fields (Camera 1 or Camera 4) too close to the Sun. Instead we study a scenario that centers Camera 3 on the ecliptic pole, which follows a similar motivation of extending the temporal baseline in the ecliptic pole region. We detail the three scenarios below:
Hemi: The third year of operation is an exact repeat of the southern hemisphere pointings from the first year.
Allsky: The spacecraft alternates observing the north and south hemisphere, with each field observed for 13.7 days instead of 27.4 days as in the primary mission.
C3PO: The spacecraft centers its camera 3 on the southern ecliptic pole, keeps its pointing in galactic latitude fixed, and changes its pointing in galactic longitude evenly between sectors.
The sky coverage of each pointing scenario is illustrated in Figure 9. The Allsky scenario has the most sky coverage but the shortest average baseline observation duration per star, while the C3PO scenario is intended to achieve the opposite.
We performed a similar planet yield simulation for each of the three extended mission pointing scenarios. For planets with orbital periods exceeding the period range in the occurrence rate table we used for the primary mission simulation, we extrapolate their occurrence rate to periods of 2,000 days assuming the planet occurrence rate follows a log uniform distribution at long periods. The results for the FFIs are shown in Figure 10. The total number of new planets expected to be discovered in the third year is of order of 2,000, with a significant number of those hosted by bright stars. The total number of new planets, as well as the multiplicity distribution at the end of the third year do not differ significantly among the three scenarios (see Figure 10). However, the C3PO pointing yields more planets with P50 days in all radius classes compared to other scenarios. This statement holds when we look at stars with brighter than 12. We do not attempt to simulate planet yields from the TPs for the extended mission, since the selection criterion of TPs may evolve significantly from the strategy we assumed for the primary mission simulation.
Given an extended mission that will last three years, we evaluate the planet yields for repeating the pointing from the third year of operation for three years. The Hemi and C3PO scenarios have a slight advantage over Allsky since the relatively long baseline allows these two scenarios to discover planets with longer periods and smaller transit depths (Figure 11). To be specific, the C3PO , Hemi and Allsky scenarios discover 300, 200 and 100 planets with and days. Depending on the scientific priorities of a TESS extended mission, one could anticipate a permutation of the above three scenarios over the three years. Additional investigation is a subject of ongoing work by the TESS Science Team, and beyond the scope of this work. Figure 13 shows that a TESS extended mission will discover a number of small planets () that are temperately irradiated and that orbit larger stars compared to the discoveries likely in the primary mission (we use the C3PO scenario as an example in that figure).
We expect a number of the single transits captured during the primary mission to be re-observed during an extended mission. However, we note that simply recovering one other transit (many orbital cycles after the first) is not sufficient to uniquely constrain the period (the period will only be constrained to a set of values such that there are an integer number of cycles between the two transits). For this reason, in order to confirm single-transit planets, it will be necessary to obtain non-TESS follow-up observations (e.g. radial velocity measurements) even for planets with re-observed transits. For each of the three scenarios, Figure 12 shows in pink the distribution of FFI planets with a single primary mission transit; those recovered during a 1-year and 3-year extended mission are layered in orange and blue, respectively. The least successful scenario in terms of the recovery of new transits for the single transit planets observed in the primary mission is C3PO. After one year, the number of single-transit planets with re-observed transits is comparable for the Hemi and Allsky scenarios. After three years, Allsky becomes the most successful scenario thanks to its coverage of both hemispheres. Most of the planets with days will not show new transits in any of the three extended mission scenarios studied here. The number of primary mission single-transit planets that remain un-observed after a three-year extended mission is 151, 396, and 530, for the Allsky, Hemi, and C3PO scenarios, respectively. The latter two numbers are dominated by planets from the un-observed hemisphere.
We note that the Hemi and C3PO scenarios are only investigated for the southern hemisphere because our knowledge of the pointing is better for the south at the current stage. Based on the estimation for the primary mission, we anticipate that an equivalent survey strategy for the northern hemisphere should produce similar results. Selection of a hemisphere may be based on the availability of follow-up resources at the time of the extended mission.
We caution the readers to be aware of the following caveats when interpreting the expected planet yields from this work.
(1) Target selection: We used a TP target list made prior to the TESS launch. In reality, the 2-minute cadence targets will be selected before the observation of each sector. The pointing plan for the northern hemisphere is more uncertain at this stage of the mission. We also do not include any GI targets (since they are not public) in the target selection process. Therefore, the targets determined to be on TESS CCDs in this work will not necessarily be observed.
(2) Stellar parameters: Stars fainter than mag have less reliable stellar parameters. We did not cross check these stars with Gaia DR2 and some of them do not have an estimated flux contamination ratio. We also caution the readers regarding the expected number of planets around late M dwarfs ( K). The planet yields around these stars are highly sensitive to the estimated stellar radii, which are not well calibrated. The radius estimation method we adopted introduces an intrinsic model dependent uncertainty on the stellar radius. Combined with the typical uncertainty of (80 K) for the low mass stars in TIC, the overall uncertainty on the radius of low mass stars is approximately .
(3) Planet injection: The injected planet population mostly reflects our understanding of the exoplanet population in the Kepler field. The occurrence rates have larger uncertainties for some parts of parameter space such as: giant planets, small planets at long periods (200 day), and planets around evolved stars. The occurrence rates we used in our simulation were not corrected for biases due to unresolved binaries in the Kepler survey (Bouma et al., 2018), nor did we simulate the effect of binaries in our study. We assumed zero eccentricity for the orbit of every planet in our simulation. For planets with a noticeable amount of eccentricity, the transit duration is more likely to be shorter, but the transit probability will be larger. A fraction of giant planets at relatively long period have non-negligible eccentricities. Our treatment tends to underestimate this giant planet population.
(4) Noise model: Our photometric noise model does not depend on stellar color. In reality, the PSF and QE of TESS have some color dependency, the amplitude of this effect will be measured in commissioning data. We also did not include potential degradation of data quality due to scattered light. Bouma et al. (2017) estimated that the scattered light effect will lead to reduction of the yield for planets by dropping the sectors suffering from Earth/Moon crossings completely, which is likely to be a upper limit. A more robust estimation on the effect of scattered light will also be estimated during commissioning.
5. Discussion and summary
We simulated planet yields for the TESS 2-year primary mission, as well as three extended mission scenarios. Our simulations take advantage of realistic constraints based on a pre-launch optical model, mission planning profile, and current best knowledge of the stars (Gaia DR2) and planets (Kepler mission) TESS is going to observe.
We report planets are likely to be discovered by the TESS primary mission, as well as an additional planets for each year of the three extended mission scenarios we explored. We predict that in the primary mission, TESS will discover about 3500 planets of Neptune size or smaller, within which, 100 will have radii smaller than . Approximately 30 of the Earth-size planets will revolve around stars brighter than 10 mag. Our estimates show that the TESS primary mission, and its extended mission will greatly expand the sample of small planets that are temperately irradiated 111111The sample is defined by , ¡1.78. To date, there are 24 planets satisfying such criteria in the exoplanet archive. At the end of a three year extended mission using the C3PO scenario, TESS is expect to find such planets, of which will revolve around F, G or K stars.
We also find that an extended TESS mission will be beneficial for recovering additional transits of planets that show only one transit in the primary mission data. The three scenarios perform differently in this respect, with the allsky and C3PO scenarios recovering the largest and smallest number of single-transiting primary mission planets, respectively.
We highlight some of the science cases where TESS planets will enable a detailed investigation.
(1) Study the density diversity of small planets: To date, there are fewer than 20 small planets () with measured density uncertainty smaller than . Typical small planets from TESS are expected to have radius uncertainties better than (given a combined constraint from Gaia and reconnaissance spectroscopy of the host star). A few hundred TESS small planets are expected to be hosted by stars with 10, potentially allowing accurate mass measurements (for slowly rotating and quiet host stars). Fulton et al. (2017), Fulton & Petigura (2018), and Berger et al. (2018) have identified a dichotomy in the radius of small planets. Obtaining the densities of planets in the same radius range will greatly enlighten the understanding of the physical origin of such a dichotomy.
(2) Study planets around small and big stars: With the next generation of infrared high precision spectrographs, it is of special interest to identify close-in planets around M dwarfs to study their properties. TESS is expected to find an order of magnitude more planets around M dwarfs than the Kepler mission. TESS will also discover many planets around the brightest and most massive stars, which will provide intriguing new opportunities to understand extreme planetary atmospheres (Shporer et al., 2014; Beatty et al., 2017; Gaudi et al., 2017).
(3) Detailed characterization of multiple planet systems: TESS will provide hundreds of new multiple transiting systems around bright stars. To date only a dozen multiple transiting planetary systems are known with host stars brighter than 12, and few have mass and other properties measured for all the planets around the same host star. Multiple-transiting planetary systems from TESS will enable follow-up observations to measure host star obliquities and individual planet densities, atmospheres, and orbital eccentricities, leading to a better understanding of planet formation and evolution.
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