Spectroscopic metallicities for planet-host stars: Extending the samples

By Nuno C. Santos, G. Israelian, M. Mayor, J. Bento, P. Almeida, Sérgio F. Sousa, A. Lisbôa, Observatoire de Geneve, Instituto de Astrof'isica de Canarias. 2005

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We present stellar parameters and metallicities for 29 planet-host stars, as well as for a large volume-limited sample of 53 stars not known to be orbited by any planetary-mass companion. These stars add to the results presented in our previous series of papers, providing two large and uniform samples of 119 planet-hosts and 94 “single” stars with accurate stellar parameters and [Fe/H] estimates. The analysis of the results further confirms that stars with planets are metal-rich when compared with average field dwarfs. Important biases that may compromise future studies are also discussed. Finally, we compare the metallicity distributions for single planet-hosts and planet-hosts in multiple stellar systems. The results show that a small difference cannot be excluded, in the sense that the latter sample is slighly overmetallic. However, more data are needed to confirm this correlation.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/9c46d4d9327b7be1ee501e6fb30b907848ff109c

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Precise radial velocities of giant stars. III. Spectroscopic stellar parameters (2007, methodology): “…directly, see for instance Valenti & Fischer (2005), or by imposing excitation and ionisation equilibrium for metal lines, using an LTE analysis and a grid of model atmospheres, see for instance Santos et al. (2004, 2005), da Silva et al. (2006), Takeda et al. (2002) and Luck & Heiter (2007).”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, background): “…Mallen-Ornelas 2005; Ford & Rasio 2006; Jones et al. 2006; Ribas & Miralda-Escudé 2007), and the incidence of giant planets as a function of host star metallicity (Fischer & Valenti 2005; Santos et al. 2005) and mass (Butler et al. 2004b; Butler et al. 2006b; Endl et al. 2006; Johnson et al. 2007).”
Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample. Revising the metallicity-planet correlation (2011, methodology): “…a spectroscopic determination for a significant number of stars within t e CORALIE sample for which we derived precise spectroscopic parameters using HARPS spectra analysed in previous work for other different planet search samples (Santos et al., 2004, 2005; Sousa et al., 2006, 2008, 2010).”
Search for brown-dwarf companions of stars (2010, unknown): “(a) Data from Santos et al. (2005).”
Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, background): “The metal-rich nature of the PHSs have been confirmed in subsequent papers (e.g. Gonzalez et al. 2001; Santos et al. 2001, 2003, 2004, 2005; Laws et al. 2003; Fischer & Valenti 2005; Gilli et al. 2006; Udry et al. 2006; Ecuvillon et al. 2007; Sousa et al. 2008; Neves et al. 2009; Johnson et al.…”
ELODIE metallicity-biased search for transiting Hot Jupiters. II. A very hot Jupiter transiting the bright K star HD 189733 (2005, background): “The main idea of the programme is to bias the target sample for high-metallicity stars which are more likely to host planets (Gonzales 1998; Santos et al. 2001, 2005; Fischer & Valenti 2005).”
The HARPS search for southern extra-solar planets - VI. A Neptune-mass planet around the nearby M dwarf Gl 581 (2005, unknown): “This contrasts with the median metallicity for solar-type stars surrounded by planets, [Fe/H]=+0.2 (Santos et al., 2005), though the significance of the difference is obviously still modest.”
Helioseismology and Solar Abundances (2007, background): “Furthermore, there is evidence that stars with planetary systems have higher heavy element abundances as compared to stars without planets (e.g., Santos et al. 2003, 2005).”
Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, background): “Interestingly, Santos et al. (2005) have found reasonably good agreement between spectroscopic and direct temperatures for four of their sample stars while Casagrande et al. (2006) have shown that the zero point of the IRFM Teff scale can be in good agreement with the spectroscopic one depending on…”
Chemical abundances of 451 stars from the HARPS GTO planet search program - Thin disc, thick disc, and planets (2009, result): “Our results are also consistent with previous studies of iron abundances (e.g. Gonzalez 1998; Gonzalez et al. 2001; Laws et al. 2003; Santos et al. 2001, 2003, 2004, 2005; Fischer & Valenti 2005), as expected.”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “Effective temperatures, surface gravities, microturbulence, and metallicity [Fe/H] were all determined by Santos et al. (2005, 2004).”
SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, methodology): “…for details on the methodology). compiling high resolution spectra to derive uniformly stellar pa- rameters and chemical abundances for stars with planetary mss companions discovered by radial velocity surveys (e.g. Santos et al. 2001, 2004b, 2005; Sousa et al. 2008, 2011b,a; Tsantaki et al. 2013).”
Spectroscopic parameters for 451 stars in the HARPS GTO planet search program - Stellar [Fe/H] and the frequency of exo-Neptunes (2008, methodology): “Stellar parameters and metallicities were derived as in previous works (Santos et al. 2004b, 2005; Sousa et al. 2006), based on the equivalent widths of Fei and Feii weak lines, by imposing excitation and ionization equilibrium.”
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.”
A new implementation of the infrared flux method using the 2MASS catalogue (2009, unknown): “Popular indirect methods for deriving effective temperatures are the excitation equilibrium of Fe i lines (e.g. Santos et al. 2004, 2005) and on fitting Balmer lines (e.g. Fuhrmann et al. 1993, 1994; Barklem et al. 2002).”
A new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in stellar Spectra (ARES) (2007, methodology): “For details on these spectra, see the work of Santos et al. (2004, 2005) and Sousa et al. (2006).”
Catalog of Nearby Exoplanets (2006, background): “; Fu4: Fuhrmann (2004); Ge5: Ge et al. (2005), http://vo.obspm.fr/exoplanets/encyclo/planet.php?p1=HD+102195&p2=b; Jh6: J. A. Johnson et al. 2006; Mc8: Marcy & Benitz (1989); Nd4: Nordström et al. (2004); Sn4: Santos, Israelian, & Mayor (2004); Sn5: Santos et al. (2005); St3: Sato et al. (2003); St”