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J/ApJ/787/47     106 Kepler ultra-short-period planets    (Sanchis-Ojeda+, 2014)

A study of the shortest-period planets found with Kepler. Sanchis-Ojeda R., Rappaport S., Winn J.N., Kotson M.C., Levine A., El Mellah I. <Astrophys. J., 787, 47 (2014)> =2014ApJ...787...47S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Effective temperatures ; Stars, diameters Keywords: planetary systems - planets and satellites: atmospheres - planets and satellites: detection Abstract: We present the results of a survey aimed at discovering and studying transiting planets with orbital periods shorter than one day (ultra-short-period, or USP, planets), using data from the Kepler spacecraft. We computed Fourier transforms of the photometric time series for all 200000 target stars, and detected transit signals based on the presence of regularly spaced sharp peaks in the Fourier spectrum. We present a list of 106 USP candidates, of which 18 have not previously been described in the literature. This list of candidates increases the number of planet candidates with orbital periods shorter than about six hours from two to seven. In addition, among the objects we studied, there are 26 USP candidates that had been previously reported in the literature which do not pass our various tests. All 106 of our candidates have passed several standard tests to rule out false positives due to eclipsing stellar systems. A low false positive rate is also implied by the relatively high fraction of candidates for which more than one transiting planet signal was detected. By assuming these multi-transit candidates represent coplanar multi-planet systems, we are able to infer that the USP planets are typically accompanied by other planets with periods in the range 1-50 days, in contrast with hot Jupiters which very rarely have companions in that same period range. Another clear pattern is that almost all USP planets are smaller than 2 R{earth}, possibly because gas giants in very tight orbits would lose their atmospheres by photoevaporation when subject to extremely strong stellar irradiation. Based on our survey statistics, USP planets exist around approximately (0.51±0.07)% of G-dwarf stars, and (0.83±0.18)% of K-dwarf stars. Description: To carry out an independent search for the shortest-period planets, we used the Kepler long-cadence time-series photometric data (30 minute samples) obtained between quarters 0 and 16. A list was prepared of all ∼200000 target stars for which photometry is available for at least one quarter, and the version 5.0 FITS files, which were available for all quarters, were downloaded from the STScI MAST Web site. For estimates of basic stellar properties including not only radii, but also masses and effective temperatures, we relied on the catalog of Huber et al. (2014, J/ApJS/211/2). This catalog is based on a compilation of photospheric properties derived from many different sources. Although it is not a homogeneous catalog, it likely provides the most accurate stellar parameters that are currently available. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 148 106 Characteristics of the 106 USP Planet Candidates Discovered in the Kepler Data
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/A+A/555/A58 : New Kepler planetary candidates (Ofir+, 2013) J/MNRAS/429/2001 : New transiting planet candidates from Kepler (Huang+, 2013) J/ApJS/211/2 : Revised stellar properties of Q1-16 Kepler targets (Huber+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1 A1 --- Group [ABC] Planet candidate group (1) 3- 10 A8 --- KIC KIC number (KIC NNNNNNNN in Simbad) 12- 18 F7.2 --- KOI KOI number (KOI -NNNN.NN in Simbad) (2) 20- 23 F4.1 mag Kpmag Kepler magnitude 25- 28 I4 K Teff Effective temperature 30- 32 I3 K E_Teff Upper limit uncertainty in Teff 34- 36 I3 K e_Teff Lower limit uncertainty in Teff 38- 41 F4.2 [cm/s2] logg Surface gravity 43- 46 F4.2 [cm/s2] E_logg Upper limit uncertainty in logg 48- 51 F4.2 [cm/s2] e_logg Lower limit uncertainty in logg 53- 56 F4.2 Rsun R* Stellar radius 58- 61 F4.2 Rsun E_R* Upper limit uncertainty in R* 63- 66 F4.2 Rsun e_R* Lower limit uncertainty in R* 68- 77 F10.8 d Porb Orbital period 79- 89 F11.6 d t0 The midtransit time (BJD-2454900) 91- 94 I4 ppm Depth Transit depth 96- 97 I2 ppm E_Depth Upper limit uncertainty in Depth 99-100 I2 ppm e_Depth Lower limit uncertainty in Depth 102-106 F5.3 h Dur Transit duration 108-112 F5.3 h E_Dur Upper limit uncertainty in Dur 114-118 F5.3 h e_Dur Lower limit uncertainty in Dur 120-123 F4.2 --- a/R* The inverse transit probability 125-128 F4.2 --- E_a/R* Upper limit uncertainty in a/R* 130-133 F4.2 --- e_a/R* Lower limit uncertainty in a/R* 135-138 F4.2 Rgeo Rp Planet radius 140-143 F4.2 Rgeo E_Rp Upper limit uncertainty in Rp 145-148 F4.2 Rgeo e_Rp Lower limit uncertainty in Rp
Note (1): Group as follows: A = New planet candidates. These objects either emerged from our search for the first time, or appear on the KOI list as false positives but that we consider to be viable candidates; B = The 69 KOIs that passed our false positive tests (Akeson et al. 2013PASP..125..989A); C = 19 other candidates that were discovered by other authors (Ofir & Dreizler 2013, J/A+A/555/A58; Huang et al. 2013, J/MNRAS/429/2001; Jackson et al. 2013ApJ...779..165J). Note (2): Planets discovered transiting stars with other KOI planets with no KOI number assigned are labeled with the KOI of the star followed by a dot and two zeros.
History: From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 23-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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