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J/AJ/153/15    Photometry and spectroscopy of EPIC 201702477    (Bayliss+, 2017)

EPIC 201702477b: a transiting brown dwarf from K2 in a 41 day orbit. Bayliss D., Hojjatpanah S., Santerne A., Dragomir D., Zhou G., Shporer A., Colon K.D., Almenara J., Armstrong D.J., Barrado D., Barros S.C.C., Bento J., Boisse I., Bouchy F., Brown D.J.A., Brown T., Cameron A., Cochran W.D., Demangeon O., Deleuil M., Diaz R.F., Fulton B., Horne K., Hebrard G., Lillo-Box J., Lovis C., Mawet D., Ngo H., Osborn H., Palle E., Petigura E., Pollacco D., Santos N., Sefako R., Siverd R., Sousa S.G., Tsantaki M. <Astron. J., 153, 15-15 (2017)> =2017AJ....153...15B (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, double and multiple ; Stars, dwarfs ; Photometry, ugriz ; Radial velocities Keywords: planetary systems - techniques: photometric - techniques: spectroscopic Abstract: We report the discovery of EPIC 201702477b, a transiting brown dwarf in a long period (40.73691±0.00037day) and eccentric (e=0.2281±0.0026) orbit. This system was initially reported as a planetary candidate based on two transit events seen in K2 Campaign 1 photometry and later validated as an exoplanet candidate. We confirm the transit and refine the ephemeris with two subsequent ground-based detections of the transit using the Las Cumbres Observatory Global Telescope 1m telescope network. We rule out any transit timing variations above the level of ∼30s. Using high precision radial velocity measurements from HARPS and SOPHIE we identify the transiting companion as a brown dwarf with a mass, radius, and bulk density of 66.9±1.7MJ, 0.757±0.065RJ, and 191±51g/cm3 respectively. EPIC 201702477b is the smallest radius brown dwarf yet discovered, with a mass just below the H-burning limit. It has the highest density of any planet, substellar mass object, or main-sequence star discovered so far. We find evidence in the set of known transiting brown dwarfs for two populations of objects-high mass brown dwarfs and low mass brown dwarfs. The higher-mass population have radii in very close agreement to theoretical models, and show a lower-mass limit around 60MJ. This may be the signature of mass-dependent ejection of systems during the formation process. Description: The Las Cumbres Observatory Global Telescope (LCOGT) is a network of fully automated telescopes. Currently there are 10 LCOGT 1m telescopes operating as part of this network, eight of which are in the southern hemisphere: three at the Cerro Tololo Inter-American Observatory (CTIO) in Chile, three at the South African Astronomical Observatory (SAAO) in South Africa, and two at Siding Spring Observatory (SSO) in Australia. Each telescope is equipped with an imaging camera; either a "Sinistro" or an SBIG STX-16803. The Sinistro is LCOGT's custom built imaging camera that features a back-illuminated 4K*4K Fairchild Imaging CCD with 15µm pixels (CCD486 BI). With a plate scale of 0.387''/pixel, the Sinistro cameras deliver a FOV of 26.6'*26.6', which is important for monitoring a sufficient number of reference stars for high-precision differential photometry. The cameras are read out by four amplifiers with 1*1 binning, with a readout time of ∼45s. The SBIG STX-16803 cameras are commercial CCD cameras which feature a frontside-illuminated 4K*4K CCD with 9µm pixels-giving a field of view of 15.8'*15.8'. These cameras are typically read out in 2*2 binning mode, which results in a read-out time of 12s. The Transiting Exoplanet CHaracterisation (TECH; lcogt.net/science/exoplanets/tech-project/) project uses the 1m telescopes in the LCOGT network to photometrically characterize transiting planets and transiting planet candidates. The first transit event for EPIC201702477b monitored by the TECH project was on 2015 March 15 from CTIO. We observed the target from 01:00 UT to 08:13 UT using a Sinistro in the r-band. The exposure times were 240s, the observing conditions were photometric, and the airmass ranged from 2.3 to 1.2. We detected a full transit of EPIC 201702477b with a depth and duration consistent with that seen in the K2 data. The next transit event occurred 41 days later on 2015 April 28, and was observable from SAAO. EPIC201702477 was monitored between 17:00 UT and 22:50 UT using an SBIG camera, again in the r-band. The exposure times were 180s, the observing conditions were again photometric, and the airmass ranged from 1.8 to 1.2. The photometric data are provided in Table1. We performed radial velocity follow-up observations of EPIC 201702477 with the SOPHIE and High-Accuracy Radial velocity Planetary Searcher (HARPS) spectrographs. Both instruments are high-resolution (R∼40000 and 110000 for SOPHIE and HARPS, respectively), fiber-fed, and environmentally controlled echelle spectrographs covering visible wavelengths. We obtained three spectra with SOPHIE (OHP programme ID:15B.PNP.HEBR) from 2015 June 12 to 2016 February 17 with exposure times of 1800 and 3600s, reaching an S/N between 8 and 22 per pixel at 5500Å. We obtained 10 other spectra with HARPS (ESO programme ID:096.C-0657) from 2016 January 10 to February 15 with exposure times between 900 and 3600s, corresponding to an S/N between 3 and 17 per pixel at 5500Å. The derived radial velocities are reported in Table3. Objects: ------------------------------------------------------------------------------- RA (ICRS) DE Designation(s) (Period) ------------------------------------------------------------------------------- 11 40 57.79 +03 40 53.7 EPIC 201702477b = NAME EPIC 201702477b (P=40.73691) ------------------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 50 192 r-band differential photometry for EPIC 201702477 from LCOGT 1m table3.dat 66 13 SOPHIE and HARPS radial velocities of EPIC 201702477
See also: J/A+A/594/A100 : K2 new planetary and EB candidates (Barros+, 2016) J/AJ/146/113 : Differential griz photometry of HATS-3 (Bayliss+, 2013) J/A+A/523/A88 : A Jupiter-mass companion around HD 109246 (Boisse+, 2010) J/A+A/505/853 : HD16760 radial velocity curve (Bouchy+, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 16 F16.10 d BJD Barycentric Julian Date (BJD-2400000) 18- 29 F12.10 --- Flux [0.985/1.007] Relative flux in the r band 31- 36 F6.4 --- e_Flux [0.0014/0.0035] Uncertainty in Flux 38- 50 A13 --- Inst Instrument used to get Flux (CTIO/Sinistro, or SAAO/SBIG) (1)
Note (1): Instruments used are defined as follows: CTIO/Sinistro = Cerro Tololo Inter-American Observatory (CTIO) using a Sinistro camera; SAAO/SBIG = South African Astronomical Observatory using a SBIG camera.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 11 F11.5 d BJD Barycentric Julian Date (BJD-2400000) 13- 18 F6.3 km/s RV [29.6/38.2] Radial velocity 20- 24 F5.3 km/s e_RV [0.007/0.06] 1σ error in RV (σRV) 26- 31 F6.3 km/s BS [-0.12/0.13] Bisector span (Vspan) 33- 37 F5.3 km/s e_BS [0.01/0.1] 1σ error in Vspan (σvspan) 39- 43 F5.3 km/s FWHM [6.3/9.7] Full Width at Half Maximum 45- 49 F5.3 km/s e_FWHM [0.013/0.12] 1σ error in FWHM (σFWHM) 51- 54 I4 s Texp [900/3600] Exposure time 56- 59 F4.1 --- S/N [2.9/21.7] Signal-to-Noise ratio (given per pixel at 550nm) 61- 66 A6 --- Inst Instrument used (SOPHIE or HARPS) (1)
Note (1): The instruments are defined as follows: SOPHIE = Spectrographe pour Observation des Phenomenes des Interieurs stellaires et des Exoplantes (literally meaning "Spectrograph for the observation of the phenomena of the stellar interiors and of the exoplanets"); HARPS = High-Accuracy Radial velocity Planetary Searcher.
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 15-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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