The HARPS search for southern extra-solar planets IX. Exoplanets orbiting HD 100777, HD 190647, and HD 221287

By D. Naef, M. Mayor, W. Benz, F. Bouchy, G. Curto, C. Lovis, C. Moutou, F. Pepe, D. Queloz, Nuno C. Santos and 1 more. 2007

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Context. The HARPS high-resolution high-accuracy spectrograph was made available to the astronomical community in the second half of 2003. Since then, we have been using this instrument for monitoring radial velocities of a large sample of Solar-type stars ($\simeq$1400 stars) in order to search for their possible low-mass companions. Aims. Amongst the goals of our survey, one is to significantly increase the number of detected extra-solar planets in a volume-limited sample to improve our knowledge of their orbital elements distributions and thus obtain better constraints for planet-formation models. Methods. Radial-velocities were obtained from high-resolution HARPS spectra via the cross-correlation method. We then searched for Keplerian signals in the obtained radial-velocity data sets. Finally, companions orbiting our sample stars were characterised using the fitted orbital parameters. Results. In this paper, we present the HARPS radial-velocity data and orbital solutions for 3 Solar-type stars: HD 100777, HD 190647, and HD 221287. The radial-velocity data of HD 100777 is best explained by the presence of a 1.16 M Jup planetary companion on a 384-day eccentric orbit ($e = 0.36$). The orbital fit obtained for the slightly evolved star HD 190647 reveals the presence of a long-period ($P = 1038$ d) 1.9 M Jup planetary companion on a moderately eccentric orbit ($e = 0.18$). HD 221287 is hosting a 3.1 M Jup planet on a 456-day orbit. The shape of this orbit is not very well-constrained because of our non-optimal temporal coverage and because of the presence of abnormally large residuals. We find clues that these large residuals result from spectral line-profile variations probably induced by processes related to stellar activity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fbcca73e2ef837e48a2427ca24a2c1f5e1336f89

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Citations in the corpus

• THE ULTRAVIOLET RADIATION ENVIRONMENT AROUND M DWARF EXOPLANET HOST STARS (2012, background): “GJ 581 has one of the richest known planetary systems, with possibly up to six planets (four confirmed) including several of Earth/super-Earth mass (Mayor et al. 2009; Tuomi 2011).”
• State of the Field: Extreme Precision Radial Velocities (2016, background): “The following cases offer a representative sample of putative planetary systems that have been debated, and the different approaches applied by the community: • GJ 581, with emphasis in the case of GJ 581d planet candidate initially described Mayor et al. (2009).”
• A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone (2013, background): “For this reason, the first super-Earth mass candidates in thehabitable zones of nearby stars have been detected around M-dwarfs (e.g. GJ 581, Mayor et al. 2009; Vogt et al. 2010)).”
• Debris disks as signposts of terrestrial planet formation (2011, background): “There are three radial zones: an inner zone containing 9 M⊕ in planetary embryos and planetesimals from 0.5 to 4 AU, three giant planets on marginally stable orbits from Jupiter’s orbital distance of 5.2 AU out to ∼10 AU (depending on the masses), and an outer 10 AU-wide disk of planetesimals contai”
• Planetary detection limits taking into account stellar noise - I. Observational strategies to reduce stellar oscillation and granulation effects (2010, background): “However, since approximately 5 years, planets from 2 to 10 M⊕, have been detected (e.g. Mayor et al. 2009b,a; Udry et al. 2007).”
• A FRAMEWORK FOR QUANTIFYING THE DEGENERACIES OF EXOPLANET INTERIOR COMPOSITIONS (2009, methodology): “As an example we use GJ 581d, a Mp sin i = 7.09 M⊕ super-Earth with a semimajor axis a = 0.22 AU that is part of a multi-planet system around an L = 0.013 L⊙ M3 dwarf star (Udry et al. 2007; Mayor et al. 2009a).”
• The HARPS search for Earth-like planets in the habitable zone - I. Very low-mass planets around HD 20794, HD 85512, and HD 192310 (2011, background): “HARPS also revealed to us the system Gl 581, with two possibly rocky planets c and d with masses of 5 and 8 MEarth, respectively, both lying at the edge of the habitable zone (HZ) of their parent star (Udry et al. 2007; Selsis et al. 2007), and the Gl 581 e of only 1.9 M⊕ (Mayor et al. 2009a).”
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• RADIAL VELOCITY PLANETS DE-ALIASED: A NEW, SHORT PERIOD FOR SUPER-EARTH 55 Cnc e (2010, background): “13, we plot the spectral window function of Mayor et al. (2009)’s new data set.”
• The HARPS search for southern extra-solar planets - XXVIII. Up to seven planets orbiting HD 10180: probing the architecture of low-mass planetary systems (2010, methodology): “Several stars from this survey have already revealed orbiting low-mass objects: HD 160691 (Santos et al. 2004; Pepe et al. 2007), HD 69830 (Lovis et al. 2006a), HD 4308 (Udry et al. 2006), HD 40307 (Mayor et al. 2009b), HD 47186, HD 181433 (Bouchy et al. 2009), and HD 90156 (Mordasini et al. 2010).”
• Search for brown-dwarf companions of stars (2010, background): “With its unmatched precision, the HARPS instrument permitted the discovery of more than 70 planetary companions to date, including earth-mass planets (e.g. Pepe et al. 2007; Santos et al. 2007; Mayor et al. 2009; Forveille et al. 2009).”
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• AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “The Geneva/HARPS planet search team reports that>30% of low-mass stars harbor planets with masses<30M⊕ on orbits shorter than 50 d (Mayor et al. 2009) and preliminaryKepler results suggest that M dwarfs host just as many, if not more, super-Earths and Neptunes as solar-mass stars (Borucki et al.…”
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• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “…below 10 M⊕ (Wolszczan & Frail 1992; McArthur et al. 2004; Santos et al. 2004; Rivera et al. 2005; Beaulieu et al. 2006; Lovis et al. 2006; Charbonneau et al. 2009; Queloz et al. 2009; Mayor et al. 2009; Batalha et al. 2011), potentially delving into the regime of true terrestrial planet formation.”
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