Spectroscopic [Fe/H] for 98 extra-solar planet-host stars. Exploring the probability of planet formation

By Nuno C. Santos, G. Israelian, M. M. O. A. D. Lisboa, P. O. D. Geneve, S. I. D. A. D. Canarias, Spain. 2003

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We present stellar parameters and metallicities, obtained from a detailed spectroscopic analysis, for a large sample of 98 stars known to be orbited by planetary mass companions (almost all known targets), as well as for a volume-limited sample of 41 stars not known to host any planet. For most of the stars the stellar parameters are revised versions of the ones presented in our previous work. However, we also present parameters for 18 stars with planets not previously published, and a compilation of stellar parameters for the remaining 4 planet-hosts for which we could not obtain a spectrum. A comparison of our stellar parameters with values of $T_{{\rm eff}}$, $\log{g}$, and [Fe/H] available in the literature shows a remarkable agreement. In particular, our spectroscopic $\log{g}$ values are now very close to trigonometric $\log{g}$ estimates based on Hipparcos parallaxes. The derived [Fe/H] values are then used to confirm the previously known result that planets are more prevalent around metal-rich stars. Furthermore, we confirm that the frequency of planets is a strongly rising function of the stellar metallicity, at least for stars with [Fe/H] > 0. While only about 3% of the solar metallicity stars in the CORALIE planet search sample were found to be orbited by a planet, this number increases to more than 25% for stars with [Fe/H] above +0.3. Curiously, our results also suggest that these percentages might remain relatively constant for values of [Fe/H] lower than about solar, increasing then linearly with the mass fraction of heavy elements. These results are discussed in the context of the theories of planetary formation.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/339630861d8b774cdca8a1b46e1e91f2010ee66e

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A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, background): “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.”
Accurate abundance patterns of solar twins and analogs - Does the anomalous solar chemical composition come from planet formation? (2009, result): “Previous studies (e.g., Smith et al. 2001; Takeda et al. 2001; Santos et al. 2004; Ecuvillon et al. 2006; Gonzalez & Laws 2007) have been cautious about reaching strong conclusions based on abundance trends withTC because of the still relatively large systematic errors associated with their…”
ON THE METAL RICHNESS OF M DWARFS WITH PLANETS (2009, background): “Abundance analyses of the stellar samples encompassed by Doppler surveys show that the occurrence rate of detectable planets correlates strongly with stellar metallicity (Santos et al. 2004; Fischer & Valenti 2005) and stellar mass (Lovis & Mayor 2007; Johnson et al. 2007).”
IMPROVED SPECTROSCOPIC PARAMETERS FOR TRANSITING PLANET HOSTS (2012, methodology): “COMPARISON WITH OTHER DETERMINATIONS Prior to this study, the largest effort to determine spectroscopic parameters for transiting planet hosts in a homogeneous way was that of Ammler-von Eiff et al. (2009), who used MOOG following the precepts of Santos et al. (2004, 2006).”
Catalog of Nearby Exoplanets (2006, neutral): “; K0: Korzennik et al. (2000); LC5: Lo Curto (2005); Le5: Lee et al. (2005); Lt9: Latham et al. (1989); Lv5: Lovis et al. (2005); MA4: McArthur et al. (2004); MC4: McCarthy et al. (2004), Mo5: Moutou et al. (2005); My3: http://obswww.unige.ch/∼naef/planet/geneva planets.html; My4: Mayor et al. (2004”
Detection Limits from the McDonald Observatory Planet Search Program (2006, background): “…surveys now routinely achieve precisions of 2-3 m s−1 (e.g. Cochran et al. 2004), facilitating the detection of ever-lower-mass companions, such as the “hot Neptunes” (Bonfils et al. 2005; McArthur et al. 2004; Santos et al. 2004b; Butler et al. 2004) and even “super-Earths” (Rivera et al. 2005).”
Accurate fundamental parameters for 23 bright solar-type stars (2010, background): “Each column is identified by the first author, i.e. Fuhrmann (1998, 2004, 2008), Sousa et al. (2008), Soubiran et al. (1998), Santos et al. (2004, 2005), and Valenti & Fischer (2005).”
Accurate fundamental parameters for lower main‐sequence stars (2006, background): “Santos et al. (2004, 2005) have carried out a detailed spectroscopic analysis for 119 planetary-host stars and 95 single stars.”
REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “For example, studies found that gas-giant planets occur more frequently around metal-rich stars (Gonzalez 1997; Santos et al. 2004; Fischer & Valenti 2005; Johnson et al. 2010).”
Effective temperature scale and bolometric corrections from 2MASS photometry (2006, methodology): “…samples of FGK stars with accurate determinations of effective temperatures (both photometric and spectroscopic) were selected from the literature (Alonso et al. 1996a; Ramírez & Meléndez 2005; Fuhrmann 1998; Santos et al. 2004; Edvardsson et al. 1993) to carry out a comparison with our results.”
Search for brown-dwarf companions of stars (2010, methodology): “The effective temperature Teff , the surface gravity log g, and the metallicity [Fe/H] are derived from the spectroscopic analysis of high-signal-to-noise spectra with the method presented in Santos et al. (2004) and using the Fe I and Fe II lines listed in Sousa et al. (2008).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, methodology): “…the three Lick/Hamilton spectra, VF05 derived Teff = 5787 ± 44K and [Fe/H] = 0.154 ± 0.029 , consistent with other LTE analyses, Teff = 5750 – 5820K and [Fe/H] = 0.14 – 0.21 (Gonzalez & Vanture 1998; Giménez 2000; Henry et al. 2000a; Santos et al. 2004; Chen & Zhao 2006; Ecuvillon et al. 2006).”
Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, background): “When compared to temperatures spectroscopically derived from the excitation balance of Fe i lines, however, a systematic difference of about 100 K is observed for metal-rich main sequence stars (e.g., Ramírez & Meléndez 2004; Santos et al. 2004; Yong et al. 2004; Heiter & Luck 2005).”
Coudé-feed stellar spectral library – atmospheric parameters (2010, background): “Beside, they compared their measurements with Edvardsson et al. (1993), Fuhrmann et al. (1997), Fuhrmann et al. (1998), Santos et al. (2004) and Allende Prieto et al. (2004), and found mean external errors of 72 K in Teff, 0.13 dex in log g, and 0.06 dex in [Fe/H].”
Five New Multicomponent Planetary Systems (2005, background): “LTE analysis of our HIRES spectra shows that ½Fe=H ¼ 0:42 (Valenti & Fischer 2005; Fischer & Valenti 2005), in good agreement with the value found by Santos et al. (2004) of 0:38 0:04 and by Laws et al. (2003) of 0:37 0:03.”
The Effective Temperature Scale of FGK Stars. I. Determination of Temperatures and Angular Diameters with the Infrared Flux Method (2005, positive): “The technique has been applied to a wide variety of samples: stars in the thin and thick disks of the Galaxy (Bensby et al. 2003, hereafter B03), planet-hosting stars (Santos et al. 2004, hereafter SIM04), globular cluster stars (Sneden et al. 2004), and so on.”
Metallicity of M dwarfs - I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence (2005, methodology): “As discussed in Santos et al. (2004, 2005), the method and the grid of ATLAS9 atmospheres used gives excellent results, compatible with those derived by other authors using other model atmospheres and methods to derive the stellar parameters and metallicities.”