J/ApJ/809/77 Transiting Exoplanet Survey Satellite (TESS) (Sullivan+, 2015)
The Transiting Exoplanet Survey Satellite: simulations of planet detections and
astrophysical false positives.
Sullivan P.W., Winn J.N., Berta-Thompson Z.K., Charbonneau D., Deming D.,
Dressing C.D., Latham D.W., Levine A.M., Mccullough P.R., Morton T.,
Ricker G.R., Vanderspek R., Woods D.
<Astrophys. J., 809, 77 (2015)>
=2015ApJ...809...77S 2015ApJ...809...77S (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Planets ; Surveys ; Photometry, infrared ;
Stars, diameters
Keywords: planets and satellites: detection; space vehicles: instruments;
surveys
Abstract:
The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored
Explorer mission that will perform a wide-field survey for planets
that transit bright host stars. Here, we predict the properties of the
transiting planets that TESS will detect along with the EB stars that
produce false-positive photometric signals. The predictions are based
on Monte Carlo simulations of the nearby population of stars,
occurrence rates of planets derived from Kepler, and models for the
photometric performance and sky coverage of the TESS cameras. We
expect that TESS will find approximately 1700 transiting planets from
2x105 pre-selected target stars. This includes 556 planets smaller
than twice the size of Earth, of which 419 are hosted by M dwarf stars
and 137 are hosted by FGK dwarfs. Approximately 130 of the
R<2R⊕ planets will have host stars brighter than Ks=9.
Approximately 48 of the planets with R<2R⊕ lie within or near
the habitable zone (0.2<S/S⊕<2); between 2 and 7 such planets
have host stars brighter than Ks=9. We also expect approximately 1100
detections of planets with radii 2-4R⊕, and 67 planets larger
than 4R⊕. Additional planets larger than 2R⊕ can be
detected around stars that are not among the pre-selected target
stars, because TESS will also deliver full-frame images at a 30-minute
cadence. The planet detections are accompanied by over 1000
astrophysical false positives. We discuss how TESS data and
ground-based observations can be used to distinguish the false
positives from genuine planets. We also discuss the prospects for
follow-up observations to measure the masses and atmospheres of the
TESS planets.
Description:
TESS will observe from a 13.7 days elliptical orbit around the Earth.
Over 2 years, it will observe the sky using 26 pointings.
The basis for our stellar population is TRILEGAL, an abbreviation for
the TRIdimensional modeL of thE GALaxy (Girardi et al.
2005A&A...436..895G 2005A&A...436..895G). TRILEGAL is a Monte Carlo population synthesis
code that models the Milky Way with four components: a thin disk, a
thick disk, a halo, and a bulge. Each of these components contains
stars with the same initial mass function but with a different spatial
distribution, star formation rate, and age-metallicity relation.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 129 1984 Catalog of simulated TESS detections
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See also:
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
J/ApJ/807/45 : Habitable zones around M dwarfs (Dressing+, 2015)
J/ApJS/210/20 : Small Kepler planets radial velocities (Marcy+, 2014)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/ApJ/772/L2 : Keck/HIRES radial velocities for HD 97658 (Dragomir+, 2013)
J/ApJ/767/95 : Improved parameters of smallest KIC stars (Dressing+, 2013)
J/A+A/552/A16 : Limb-darkening for CoRoT, Kepler, Spitzer. II. (Claret+, 2013)
J/ApJ/757/112 : Stellar diameters. II. K and M-stars (Boyajian+, 2012)
J/A+A/546/A14 : Limb-darkening for CoRoT, Kepler, Spitzer (Claret+, 2012)
J/AJ/142/160 : Kepler Mission. II. eclipsing binaries (Slawson+, 2011)
J/AJ/141/83 : Eclipsing binaries in Kepler first data release (Prsa+, 2011)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/MNRAS/389/869 : Multiplicity among bright stellar systems (Eggleton+, 2008)
J/AJ/133/439 : Luminosity function of M7-L8 ultracool dwarfs (Cruz+, 2007)
J/A+A/392/741 : Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)
J/A+AS/141/371 : Low-mass stars evolutionary tracks+isochrones (Girardi+, 2000)
J/PASP/110/863 : A Stellar Spectral Flux Library: 1150 - 25000 A (Pickles 1998)
http://stev.oapd.inaf.it/cgi-bin/trilegal : TRILEGAL 1.6 input form
http://www.astro.keele.ac.uk/jkt/debcat : Catalog of Eclipsing Binaries
http://keplerebs.villanova.edu/v2 : Kepler EB catalog
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 8 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000)
10- 18 F9.5 deg DEdeg Declination in decimal degrees (J2000)
20- 26 F7.4 Rgeo Rp [0.6/22] Planetary radius in Earth units
28- 35 F8.4 d Per [0.5/225] Period
37- 45 E9.3 --- S [0.07/55380] Planetary insolation in Earth units
47- 53 F7.4 m/s K [0.3/28.1] Radial-velocity semiamplitude
55- 60 F6.4 Rsun R* [0.1/4.1] Stellar radius
62- 70 E9.3 K Teff [2529/11910] Stellar effective temperature
72- 77 F6.3 mag Vmag [4.2/19.2] Apparent V band magnitude
79- 84 F6.3 mag Imag [3.7/16.7] Apparent IC band magnitude
86- 91 F6.3 mag Jmag [3.3/15.3] Apparent J band magnitude
93- 98 F6.3 mag Ksmag [3/14.5] Apparent Ks band magnitude
100-104 F5.2 mag DM [-2.1/8.4] Distance Modulus
106-111 F6.3 --- Dil [1/40.7] Dilution parameter for all detected
eclipses
113-118 F6.3 [-] logsigV [-5.1/-2.4] Log standard deviation in
relative flux (1)
120-127 F8.3 --- SNR [7.3/1188] Signal-to-Noise Ratio
129 I1 --- Mult [0/4] Number of other planets orbiting the star
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Note (1): Due to stellar variability, after phase-folding all of the
transits together.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 07-Dec-2015