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J/MNRAS/460/3706      Radial velocity curves of ν Oct           (Ramm+, 2016)

The conjectured S-type retrograde planet in ν Octantis: more evidence including four years of iodine-cell radial velocities. Ramm D.J., Nelson B.E., Endl M., Hearnshaw J.B., Wittenmyer R.A., Gunn F., Bergmann C., Kilmartin P., Brogt E. <Mon. Not. R. Astron. Soc., 460, 3706-3719 (2016)> =2016MNRAS.460.3706R (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Radial velocities Keywords: techniques: radial velocities - planets and satellites: dynamical evolution and stability - binaries: spectroscopic - stars: individual: nu Oct Abstract: We report 1212 radial-velocity (RV) measurements obtained in the years 2009-2013 using an iodine cell for the spectroscopic binary ν Octantis (K1 III/IV). This system (abin∼2.6au, P∼1050d) is conjectured to have a Jovian planet with a semimajor axis half that of the binary host. The extreme geometry only permits long-term stability if the planet is in a retrograde orbit. Whilst the reality of the planet (P∼415d) remains uncertain, other scenarios (stellar variability or apsidal motion caused by a yet unobserved third star) continue to appear substantially less credible based on cross-correlation function bisectors, line-depth ratios and many other independent details. If this evidence is validated but the planet is disproved, the claims of other planets using RVs will be seriously challenged. We also describe a significant revision to the previously published RVs and the full set of 1437 RVs now encompasses nearly 13 yr. The sensitive orbital dynamics allow us to constrain the 3D architecture with a broad prior probability distribution on the mutual inclination, which with posterior samples obtained from an N-body Markov chain Monte Carlo is found to be 152.5+0.7-0.6°. None of these samples are dynamically stable beyond 106yr. However, a grid search around the best-fitting solution finds a region that has many models stable for 107yr, and includes one model within 1σ that is stable for at least 108yr. The planet's exceptional nature demands robust independent verification and makes the theoretical understanding of its formation a worthy challenge. Description: All spectroscopic observations were obtained at University of Canterbury Mt John Observatory, Lake Tekapo, New Zealand using the 1-m McLellan telescope and the echelle spectrograph HERCULES. From the start of operations in 2001 until 2006/7 the detector was a 1kx1k detector. Initial testing of a complete-wavelength-coverage 4kx4k detector began in 2006 October. This detector was then removed briefly and the original detector used until the 4kx4k CCD was installed permanently in early 2007. Objects: ------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------- 21 41 28.65 -77 23 24.2 nu Oct = HR 8254 ------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 48 1180 List of the 1180 austral-processed I2 spectra acquired during 2009-2013 using the 4kx4k CCD table4.dat 48 32 List of the relative velocity data of 32 4kx4k detector observations acquired 2006-2013 using CCF fitting table5.dat 48 225 List of the 225 spectra acquired during 2001-2007 using the 1kx1k CCD
Byte-by-byte Description of file: table3.dat table4.dat table5.dat
Bytes Format Units Label Explanations
1- 9 F9.4 d JD Barycentric-corrected Julian date (JD-2450000) 13- 19 F7.3 km/s VI2 Corrected I2 relative radial velocity 24- 27 F4.1 m/s e_VI2 Internal error on VI2 (σi) 31- 38 F8.4 km/s bary.corr Barycentric correction 46- 48 I3 --- S/N Signal-to-noise ration in order n=110
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 24-Nov-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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