Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample. Revising the metallicity-planet correlation

By Sérgio F. Sousa, Nuno C. Santos, G. Israelian, M. Mayor, S. M. C. D. Astrof'isica, U. Porto, Instituto de Astrof'isica de Canarias, G. Observatory, Geneva University, D. D. Astronomia and 3 more. 2011

221 citations recorded by the source corpus.

To understand the formation and evolution of solar-type stars and planets in the solar neighborhood, we need to obtain their stellar parameters with high precision. We present a catalog of precise stellar parameters for low-activity FGK single stars in a volumelimited sample followed by the HARPS spectrograph in the quest to identify extra-solar planets. The spectroscopic analysis was completed assuming LTE with a grid of Kurucz atmosphere models and using the ARES code to perform an automatic measurement of the line equivalent widths. The results are compared with different independent methods and also with other values found in the literature for common stars. Both comparisons are consistent and illustrate the homogeneity of the parameters derived by our team. The derived metallicities of this sample reveal a somewhat different distribution for the present planet hosts, but still indicates the already known higher frequency of planets observed for the more metal-rich stars. We combine the results derived in this sample with the one from the CORALIE survey to present the largest homogeneous spectroscopic study of the metallicity-giant-planet relation using a total of 1830 stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e21d2e9b803b245615e5c2e86e9ee277bff83dc6

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In Astronomy and Astrophysics

1. D. Charbonneau
2. C. Mordasini
3. J. Southworth
4. E. Gaidos
5. Jon Fortney
6. Nuno C. Santos
7. J. Johnson
8. A. Mann

In Instrumentation

1. D. Charbonneau
2. E. Gaidos
3. J. Southworth
4. A. Mann
5. C. Mordasini
6. Nuno C. Santos
7. J. Johnson
8. M. Mayor

Citations in the corpus

• GIANT PLANETS ORBITING METAL-RICH STARS SHOW SIGNATURES OF PLANET–PLANET INTERACTIONS (2013, background): “Independent and follow-up studies confirmed this trend for giant planets (e.g. Fischer & Valenti 2005, Sozzetti et al. 2009 Johnson et al. 2010, Sousa et al. 2011, Mortier et al. 2012) but not small planets (Ribas & Miralda-Escudé 2007; Buchhave et al. 2012).”
• PROSPECTING IN LATE-TYPE DWARFS: A CALIBRATION OF INFRARED AND VISIBLE SPECTROSCOPIC METALLICITIES OF LATE K AND M DWARFS SPANNING 1.5 dex (2012, background): “Errors for individual stars listed in Table 2. cMetallicities determined from Strömgren photometry. dBased on a control sample from Santos et al. (2004) and Sousa et al. (2011), on which abundances in N12 are anchored. of TiO and CaH bands (Reid et al. 1995).”
• NEAR-INFRARED METALLICITIES, RADIAL VELOCITIES, AND SPECTRAL TYPES FOR 447 NEARBY M DWARFS (2013, result): “Our findings are consistent with those from Sousa et al. (2011) and Sozzetti et al. (2009).”
• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, result): “This result was subsequently discussed in several studies (e.g. Sousa et al. 2008; Ghezzi et al. 2010) and recently confirmed (Mayor et al. 2011; Sousa et al. 2011).”
• The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, result): “Sousa et al. (2011) compared stars that are in common with this sample and various other samples (Edvardsson et al. 1993; Bensby et al. 2003; Valenti & Fischer 2005), showing that there is no systematic difference in these analyses for [Fe/H] or Teff for stars with Teff < 6000 K, but found a…”
• The PASTEL catalogue: 2016 version (2016, background): “Since 2010, eleven papers have published more than 250 (Teff , log g, [Fe/H]) determinations, and four papers present more than 500 stars (Bensby et al. 2014; Luck 2014; Ramírez et al. 2013; Sousa et al. 2011).”
• REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, methodology): “To find the fraction of stars with ⩽T 5650eff K, we checked the HARPS FKG star sample (Sousa et al. 2011), 55% of stars in the sample have Teff lower than 5650 K.”
• Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program - Galactic stellar populations and planets (2012, methodology): “This result confirms the “metal-poor“ nature (e.g. Udry & Santos 2007; Sousa et al. 2008, 2011a; Mayor et al. 2011) of low-mass planet hosts, when extended to elements other than iron.”
• SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, methodology): “For cases where the parallax is not available, we computed a “spectroscopic parallax” using the estimated stellar parameters (for details on the method we point to Sousa et al. 2011a).”
• THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET (2014, methodology): “We adopted the line list from Sousa et al. (2011), but the oscillator strength values log gf were re-determined by 17 Available at http://kurucz.harvard.edu/grids.html. inverse analysis of their solar EWs using an Iron abundance of log (Fe) = 7.52 (and the other photospheric parameters unchanged),…”
• Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “Unfortunately, techniques such as radial velocity variability or microlensing, which have yielded many planets (Sousa et al., 2011), only detect planets out to a few AU.”
• AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, background): “While gas-giant planets appear to form preferentially around metal-rich stars, small planets (with radii less than 4R⊕) can form under a wide range of metallicities (Sousa et al. 2011; Buchhave et al. 2012, 2014).”
• SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, background): “We also confirm that the EGP – host metallicity correlation previously found by RV surveys (e.g. Sousa et al. 2011; Johnson et al. 2012; Mortier et al. 2013) holds for the transit exoplanet population in the Kepler field.”