J/MNRAS/475/3090 Predicted properties for 468 RV planets (Yi+, 2018)
Forecasting the detectability of known radial velocity planets with the
upcoming CHEOPS mission.
Yi J.S., Chen J., Kipping D.
<Mon. Not. R. Astron. Soc., 475, 3090-3097 (2018)>
=2018MNRAS.475.3090Y 2018MNRAS.475.3090Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, masses ;
Stars, diameters
Keywords: methods: statistical - eclipses - planets and satellites: detection
Abstract:
The CHaracterizing ExOPlanets Satellite (CHEOPS) mission is planned
for launch next year with a major objective being to search for
transits of known radial velocity (RV) planets, particularly those
orbiting bright stars. Since the RV method is only sensitive to
planetary mass, the radii, transit depths and transit signal-to-noise
values of each RV planet are, a priori, unknown. Using an empirically
calibrated probabilistic mass-radius relation, forecaster, we address
this by predicting a catalogue of homogeneous credible intervals for
these three keys terms for 468 planets discovered via RVs. Of these,
we find that the vast majority should be detectable with CHEOPS,
including terrestrial bodies, if they have the correct geometric
alignment. In particular, we predict that 22 mini-Neptunes and 82
Neptune-sized planets would be suitable for detection and that more
than 80 per cent of these will have apparent magnitude of V<10,
making them highly suitable for follow-up characterization work. Our
work aims to assist the CHEOPS team in scheduling efforts and
highlights the great value of quantifiable, statistically robust
estimates for upcoming exoplanetary missions.
Description:
In this work, we have predicted the planetary radii, transit depths,
and associated SNRs using CHEOPS (Broeg et al., 2013, CHEOPS: A
transit photometry mission for ESA's small mission programme, EPJ Web
Conf., 47, 3005) for 468 planets listed on the "exoplanet Orbit
Database" (EOD; Han et al., 2014PASP..126..827H 2014PASP..126..827H, Exoplanets.org) as
having been discovered using the RV method. Our SNR values assume 1h
of cumulative integration time, no intrinsic stellar noise, employ a
CHEOPS noise model dependent on spectral type and apparent magnitude,
and accounts for instrument saturation.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 534 468 Final predicted properties for 468 RV planets
using forecaster
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Planet name
18- 38 F21.16 Mgeo Mass Planetary mass
40- 63 F24.17 Mgeo e_Mass Planetary mass ±34.1% uncertainty
65- 82 F18.16 Rgeo Rad2.2 Planetary radius 2.2% quantile
84-102 F19.16 Rgeo Rad15.9 Planetary radius 15.9% quantile
104-122 F19.16 Rgeo Rad50.0 Planetary radius 50.0% quantile
124-142 F19.16 Rgeo Rad81.1 Planetary radius 84.1% quantile
144-162 F19.16 Rgeo Rad97.7 Planetary radius 97.7% quantile
164-172 F9.6 Rsun Rad* Stellar radius
174-193 F20.18 Rsun e_Rad* Stellar radius -34.1% uncertainty
195-203 F9.7 Rsun E_Rad* Stellar radius +34.1% uncertainty
205-226 F22.19 10-3 Depht2.2 Transit depth 2.2% quantile
(in parts per thousand unit)
228-250 F23.19 10-3 Depht15.9 Transit depth 15.9% quantile
(in parts per thousand unit)
252-273 F22.18 10-3 Depht50.0 Transit depth 50.0% quantile
(in parts per thousand unit)
275-296 F22.18 10-3 Depht84.1 Transit depth 84.1% quantile
(in parts per thousand unit)
298-319 F22.18 10-3 Depht97.7 Transit depth 97.7% quantile
(in parts per thousand unit)
321-327 F7.4 mag Vmag V-band apparent magnitude
329-349 E21.17 ppm/h phnoise CHEOPS r.m.s. photometric noise
(in parts per million/hour unit)
351-371 E21.17 ppm/h phnoise2.2 CHEOPS signal-to-noise ratio per hour 2.2%
quantile (in parts per million/hour unit)
373-392 E20.17 ppm/h phnoise15.9 CHEOPS signal-to-noise ratio per hour 15.9%
quantile (in parts per million/hour unit)
394-414 E21.17 ppm/h phnoise50.0 CHEOPS signal-to-noise ratio per hour 50.0%
quantile (in parts per million/hour unit)
416-436 E21.17 ppm/h phnoise84.1 CHEOPS signal-to-noise ratio per hour 84.1%
quantile (in parts per million/hour unit)
438-457 E20.17 ppm/h phnoise97.7 CHEOPS signal-to-noise ratio per hour 97.7%
quantile (in parts per million/hour unit)
459-478 F20.16 h Dur Maximum transit duration [hours]
480-501 F22.18 h e_Dur Maximum transit duration -34.1% uncertainty
503-524 F22.18 h E_Dur Maximum transit duration +34.1% uncertainty
526-532 F7.4 % Prob ?=- Geometric transit probability
534 I1 --- Flag [0/3] Planet flag (1)
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Note (1): Planet flag as follows:
0 = No remarks
1 = No stellar radii was reported on EOD and the EOD reported maximum
a-posteriori stellar mass was below 0.87 Solar masses enabling a
forecaster stellar radius prediction. Forecaster prediction used
the reported stellar mass uncertainty assuming a Gaussian.
2 = No stellar radii was reported on EOD and the EOD reported maximum
a-posteriori stellar mass was below 0.87 Solar masses enabling a
forecaster stellar radius prediction. Forecaster prediction could
not use the reported stellar mass uncertainty, since none existed,
and thus we assumed a Gaussian of width equal to 5.0% of the best
reported stellar mass.
3 = Object has an EOD reported maximum a-posteriori stellar radius but
no associated uncertainty. Uncertainty was therefore assumed to be
equal to 3.5% of the maximum a-posteriori value and Gaussian.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Apr-2021