The Transiting Exoplanet Survey Satellite: Simulations of Planet Detections and Astrophysical False Positives

Sullivan, Peter; Winn, Joshua N.; Berta-Thompson, Zachory K.; Charbonneau, David; Deming, Drake; Dressing, Courtney D.; Latham, David W.; Levine, Alan M.; McCullough, P. R.; Morton, Timothy; Ricker, G.; Vanderspek, R.; Woods, D.

doi:10.1088/0004-637x/809/1/77

Cited by 512 publications

(712 citation statements)

References 82 publications

Supporting

Mentioning

685

Contrasting

Unclassified

Order By: Relevance

“…The K2 mission (Howell et al 2014) might identify more short-period planets within several nearby young stellar associations 6 . TESS (Ricker et al 2015;Sullivan et al 2015) can search for planets with a much larger range of orbital periods.…”

Section: Testing the Possibilitiesmentioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

View full text Add to dashboard Cite

We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earthmass planets around mature solar-type stars based on exoplanet surveys (∼ 20%) stands in stark contrast to the low incidence rate (≤ 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (∼ 10 Myr). If Earth-mass planets at AU distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density 10 −5 of the minimum mass solar nebula.

show abstract

Section: Testing the Possibilitiesmentioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

View full text Add to dashboard Cite

show abstract

“…Studies of TESS planet yield suggest more than 100 single transits could be detected above a noise threshold of 7.3σ (Sullivan et al 2015). Namaste could be an important tool in the follow-up of these planets.…”

Section: Application To Future Missionsmentioning

confidence: 99%

Single transit candidates from K2: detection and period estimation

Osborn

Armstrong

Brown

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Photometric surveys such as Kepler have the precision to identify exoplanet and eclipsing binary candidates from only a single transit. K2, with its 75 d campaign duration, is ideally suited to detect significant numbers of single-eclipsing objects. Here we develop a Bayesian transit-fitting tool ('Namaste: An Mcmc Analysis of Single Transit Exoplanets') to extract orbital information from single transit events. We achieve favourable results testing this technique on known Kepler planets, and apply the technique to seven candidates identified from a targeted search of K2 campaigns 1, 2 and 3. We find EPIC203311200 to host an excellent exoplanet candidate with a period, assuming zero eccentricity, of 540 +410 −230 d and a radius of 0.51 ± 0.05R Jup . We also find six further transit candidates for which more follow-up is required to determine a planetary origin. Such a technique could be used in the future with TESS, PLATO and ground-based photometric surveys such as NGTS, potentially allowing the detection of planets in reach of confirmation by Gaia.

show abstract

“…The DHS also enables characterization of any future targets found in this brightness range, such as by the Transiting Exoplanet Survey Satellite (TESS) (Ricker et al 2014). We plot the expected yield of TESS (Sullivan et al 2015) in Figure 8 and none of the simulated targets saturate the DHS. TESS Sim Known Systems Figure 8.…”

Section: Brightness Limitsmentioning

confidence: 99%

“…The magnitudes are Vega K S magnitudes where 80% of the well depth is filled in the standard CDS readout mode (described in Figure 5) for a 2048 × 64 pixel sub-array using 4 amplifiers. The blue points are known transiting systems and the green points are simulated TESS planets (Sullivan et al 2015).…”

Section: Brightness Limitsmentioning

confidence: 99%

Two NIRCam Channels are Better than One: HowJWSTCan Do More Science with NIRCam’s Short-wavelength Dispersed Hartmann Sensor

Schlawin¹,

Rieke²,

Leisenring³

et al. 2016

PASP

View full text Add to dashboard Cite

The James Webb Space Telescope (JWST) offers unprecedented sensitivity, stability, and wavelength coverage for transiting exoplanet studies, opening up new avenues for measuring atmospheric abundances, structure, and temperature profiles. Taking full advantage of JWST spectroscopy of planets from 0.6µm to 28µm, however, will require many observations with a combination of the NIRISS, NIRCam, NIRSpec, and MIRI instruments. In this white paper, we discuss a new NIRCam mode (not yet approved or implemented) that can reduce the number of necessary observations to cover the 1.0µm to 5.0µm wavelength range. Even though NIRCam was designed primarily as an imager, it also includes several grisms for phasing and aligning JWST's 18 hexagonal mirror segments. NIRCam's long-wavelength channel includes grisms that cover 2.4µm to 5.0µm with a resolving power of R = 1200 − 1550 using two separate configurations. The long-wavelength grisms have already been approved for science operations, including wide field and single object (time series) slitless spectroscopy. We propose a new mode that will simultaneously measure spectra for science targets in the 1.0µm to 2.0µm range using NIRCam's short-wavelength channel. This mode, if approved, would take advantage of NIRCam's Dispersed Hartmann Sensor (DHS), which produces 10 spatially separated spectra per source at R ∼ 300. We discuss the added benefit of the DHS in constraining abundances in exoplanet atmospheres as well as its ability to observe the brightest systems. The DHS essentially comes for free (at no time cost) with any NIRCam long-wavelength grism observation, but the detector integration parameters have to be selected to ensure that the long-wavelength grism observations do not saturate and that JWST data volume downlink constraints are not violated. Combining both of NIRCam's channels will maximize the science potential of JWST, which is a limited life observatory.

show abstract

The Transiting Exoplanet Survey Satellite: Simulations of Planet Detections and Astrophysical False Positives

Cited by 512 publications

References 82 publications

Rocky Planet Formation: Quick and Neat

Rocky Planet Formation: Quick and Neat

Single transit candidates from K2: detection and period estimation

Two NIRCam Channels are Better than One: HowJWSTCan Do More Science with NIRCam’s Short-wavelength Dispersed Hartmann Sensor

Contact Info

Product

Resources

About