J/AJ/157/235 Observations of the Kepler field with TESS (Christ+, 2019)
Observations of the Kepler field with TESS: predictions for planet yield
and observable features.
Christ C.N., Montet B.T., Fabrycky D.C.
<Astron. J., 157, 235 (2019)>
=2019AJ....157..235C 2019AJ....157..235C (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets ; Magnitudes ; Stars, masses ; Models
Keywords: methods: data analysis - planet-star interactions -
planetary systems -
planets and satellites: individual (KOI-142 b/Kepler-88 b)
Abstract:
We examine the ability of the Transiting Exoplanet Survey Satellite (TESS)
to detect and improve our understanding of planetary systems in the Kepler
field. By modeling the expected transits of all confirmed and candidate
planets detected by Kepler as expected to be observed by TESS, we provide
a probabilistic forecast of the detection of each Kepler planet in TESS
data. We find that TESS has a greater than 50% chance of detecting 260
of these planets at the 3σ level in one sector of observations and
an additional 120 planets in two sectors. Most of these are large planets
in short orbits around their host stars, although a small number of rocky
planets are expected to be recovered. Most of these systems have only
one known transiting planet; in only ∼5% of known multiply transiting
systems do we anticipate more than one planet to be recovered. When these
planets are recovered, we expect TESS to be a powerful tool to characterize
transit timing variations. Using Kepler-88 (KOI-142) as an example, we
show that TESS will improve measurements of planet-star mass ratios and
orbital parameters, and significantly reduce the transit timing uncertainty
in future years. Because TESS will be most sensitive to hot Jupiters, we
research whether TESS will be able to detect tidal orbital decay in these
systems. We find two confirmed planetary systems (Kepler-2 b and
Kepler-13 b) and five candidate systems that will be good candidates
to detect tidal decay.
Description:
We use the stellar and planetary properties from Mathur et al. (2017,
J/ApJS/229/30) for systems in the NASA Exoplanet Archive to determine
the types of planets TESS will be sensitive to. We consider planets
labeled as "confirmed" or "candidate", and ignore any systems identified
as false positives. We contaminate the transit depths from Thompson et al.
(2018, J/ApJS/235/38) with TESS's contamination ratios (Stassun et al.
2018, J/AJ/156/102) to find the transit depths that TESS is expected
to observe for each system. At the 3σ level, there are 154 (232)
confirmed and 106 (148) candidate planets that are detectable in one (two)
sector(s). In total, we expect TESS is likely to recover 260 (380) of
these signals originally detected by Kepler in one (two) sectors.
Objects:
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RA (ICRS) DE Designation(s)
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19 24 35.54 +40 40 09.8 KOI-142 = Kepler-88
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 71 380 A list of expected signals and computed
probabilities of detection at the 3σ level
for both one and two sectors of observation
table4.dat 73 364 List of parameter and critical Q* values for
all detectable systems at the 3σ level in
two sectors
kep.dat 124 30000 KOI-142 planetary parameters using all of the
Kepler data available to the public
keptess.dat 124 30000 KOI-142's planetary parameters using all of the
Kepler data available to the public as well as
a theoretical TESS data point in July 2019
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See also:
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/ApJ/809/77 : Transiting Exoplanet Survey Satellite (TESS) (Sullivan+, 2015)
J/ApJS/229/30 : Revised stellar properties of Q1-17 Kepler targets
(Mathur+, 2017)
J/AJ/156/102 : The TESS Input Catalog and Candidate Target List
(Stassun+, 2018)
J/ApJS/235/38 : Kepler planetary cand. VIII. DR25 reliability (Thompson+, 2018)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- KOI Kepler Object of Interest number (KNNNNN.NN)
11- 24 A14 --- Kepler Kepler name
26- 30 F5.2 mag Tessmag [7.58/15.97] TESS apparent magnitude (1)
32- 37 I6 ppm Tdepth [28/146626] Calculated TESS transit depth (2)
39- 43 I5 ppm TotNoise [117/10741] Calculated total noise (3)
45- 51 F7.2 --- S/N1 [1.27/1481.26] Signal-to-noise ratio for one
sector
53- 59 F7.2 --- S/N2 [2.53/2094.96] Signal-to-noise ratio for two
sectors
61- 65 F5.3 --- Prob1 [0.193/1.0] Probability of detection for one
sector
67- 71 F5.3 --- Prob2 [0.501/1.0] Probability of detection for two
sectors
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Note (1): Taken from Stassun et al. (2018, J/AJ/156/102).
Note (2): Calculated using Kepler and TESS contamination ratios from
Brown et al. (2011, J/AJ/142/112) and Stassun et al. (2018, J/AJ/156/102),
respectively.
Note (3): Obtained by inputting TESS apparent magnitudes into the function
from Sullivan et al.'s Fig. 14 (2015, J/ApJ/809/77).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- KOI Kepler Object of Interest number (KNNNNN.NN)
11- 24 A14 --- Kepler Kepler name
26- 35 F10.6 d Per [0.453287/105.881767] Period of planet
37- 41 F5.2 Rgeo Rp [0.5/29.91] Radius of planet
43- 46 F4.2 Msun M* [0.09/3.26] Mass of host star
48- 54 F7.2 min sigKep [0.06/3789.88]? Calculated Kepler transit
uncertainty
56- 61 F6.2 min sigTESS [0.04/368.85] Calculated TESS transit
uncertainty
63- 67 F5.2 [-] RmQ [-6.79/7.34]? Q, tidal quality parameter of host
star (1)
69- 73 F5.2 [-] JupQ [-5.93/7.34]? Q, tidal quality parameter of host
star (2)
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Note (1): Calculated using planet masses obtained from the mass-radius relation
for planets with radii <8 R⊕. Otherwise, assumed planets with
radii ≥8 R⊕ to be Jupiter mass planets.
Note (2): Assumed that all planets are one Jupiter mass.
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Byte-by-byte Description of file: kep.dat keptess.dat
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Bytes Format Units Label Explanations
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1- 11 E11.6 Msun Mass-b [1.67452e-07/4.24705e-05] Mass for the innermost
planet (mass_b)
13- 20 F8.5 d Per-b [10.9158/10.9175] Period for the innermost
planet (period_b)
22- 28 F7.5 --- e-b [0.05458/0.05643] Eccentricity for the innermost
planet (e_b)
30- 37 F8.5 deg i-b [87.8941/89.9054] Inclination for the innermost
planet (i_b)
39- 47 F9.5 deg omega-b [173.65/183.957] Argument of periastron for
the innermost planet ω (omega_b)
49- 57 F9.5 deg lambda-b [259.176/269.22] Mean longitude for the
innermost planet λ (lambda_b)
59- 69 E11.6 Msun Mass-c [6.05650e-04/6.44979e-04] Mass for the outermost
planet (mass_c)
71- 78 F8.5 d Per-c [22.2597/22.2704] Period for the outermost
planet (period_c)
80- 86 F7.5 --- e-c [0.05525/0.05931] Eccentricity for the outermost
planet (e_c)
88- 95 F8.5 deg i-c [83.9864/91.1843] Inclination for the outermost
planet (i_c)
97-105 F9.5 deg omega-c [353.043/365.774] Argument of periastron for
the outermost planet ω (omega_c)
107-114 F8.5 deg Long-c [-1.73898/3.34495] Longitude of the ascending
node for the outermost planet (longnode_c)
116-124 F9.5 deg lambda-c [331.771/340.005] Mean longitude for the
outermost planet λ (lambda_c)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 21-Aug-2019