S4N: A spectroscopic survey of stars in the solar neighborhood: The nearest 15 pc

By C. Allende Prieto, Paul Barklem, D. Lambert, K. Texas, Usa Uppsala Astronomical Observatory, Sweden., O. Nacional, Brazil. 2004

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We report the results of a high-resolution spectroscopic survey of all the stars more luminous than M V = 6.5 mag within 14.5 pc from the Sun. The Hipparcos catalog's completeness limits guarantee that our survey is comprehensive and free from some of the selection effects in other samples of nearby stars. The resulting spectroscopic database, which we have made publicly available, includes spectra for 118 stars obtained with a resolving power of $R \simeq 50\,000$, continuous spectral coverage between ${\sim} 362{-}921$ nm, and typical signal-to-noise ratios in the range $150{-}600$. We derive stellar parameters and perform a preliminary abundance and kinematic analysis of the F-G-K stars in the sample. The inferred metallicity ([Fe/H]) distribution is centered at about -0.1 dex, and shows a standard deviation of 0.2 dex. A comparison with larger samples of Hipparcos stars, some of which have been part of previous abundance studies, suggests that our limited sample is representative of a larger volume of the local thin disk. We identify a number of metal-rich K-type stars which appear to be very old, confirming the claims for the existence of such stars in the solar neighborhood. With atmospheric effective temperatures and gravities derived independently of the spectra, we find that our classical LTE model-atmosphere analysis of metal-rich (and mainly K-type) stars provides discrepant abundances from neutral and ionized lines of several metals. This ionization imbalance could be a sign of departures from LTE or inhomogeneous structure, which are ignored in the interpretation of the spectra. Alternatively, but seemingly unlikely, the mismatch could be explained by systematic errors in the scale of effective temperatures. Based on transitions of majority species, we discuss abundances of 16 chemical elements. In agreement with earlier studies we find that the abundance ratios to iron of Si, Sc, Ti, Co, and Zn become smaller as the iron abundance increases until approaching the solar values, but the trends reverse for higher iron abundances. At any given metallicity, stars with a low galactic rotational velocity tend to have high abundances of Mg, Si, Ca, Sc, Ti, Co, Zn, and Eu, but low abundances of Ba, Ce, and Nd. The Sun appears deficient by roughly 0.1 dex in O, Si, Ca, Sc, Ti, Y, Ce, Nd, and Eu, compared to its immediate neighbors with similar iron abundances.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/16b6adaa89a560568241e828903ce7dcfa959952

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Citations in the corpus

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs (2005, background): “This assumption neglects the possibility that the Sun itself may have peculiar abundances (e.g., Allende Prieto et al. 2004).”
Chemical abundances of 451 stars from the HARPS GTO planet search program - Thin disc, thick disc, and planets (2009, unknown): “…(2005), Gilli et al. (2006), Gonzalez & Laws (2007), and Takeda (2007) (hereafter SAD, BOD, BEI, FV05, GIL, GZ07, and TAK, respectively), as well as other reference studies by Chen et al. (2000), Allende Prieto et al. (2004), and Bensby et al. (2005) (hereafter CH00, AP04, and BEN, respectively).”
THE MILKY WAY'S CIRCULAR-VELOCITY CURVE BETWEEN 4 AND 14 kpc FROM APOGEE DATA (2012, background): “REFERENCES Allende Prieto, C., Barklem, P. S., Lambert, D. L., & Cunha, K. 2004, A&A, 420, 183 Aumer, M. & Binney, J. J. 2009, MNRAS, 397, 1286 Bensby, T., Oey, M. S., Feltzing, S., & Gustafsson, B. 2007, ApJ, 655, 89 Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., & Nasi, E. 1994, A&AS, 106, 27”
THE MILKY WAY TOMOGRAPHY WITH SDSS. III. STELLAR KINEMATICS (2009, methodology): “Values of Hμ in the range 350–700 pc are consistent with the data—the decrease in Hμ is required by the local constraint, μD(Z) = −0.2 (Nordström et al. 2004; Allende Prieto et al. 2004).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “Ten or more Gaia FGK benchmark stars were analysed spectroscopically by Valenti & Fischer (2005), Luck & Heiter (2005), and Bruntt et al. (2010), while the parallax method was applied for more than ten stars by Allende Prieto et al. (2004) and Ramírez et al. (2007).”
The Solar Twin Planet Search. I. Fundamental parameters of the stellar sample (2014, methodology): “We also added more targets from our spectroscopic analysis of solar twins fromthe S4N database (Allende Prieto et al. 2004) and the HARPS/ESO archive, as reported in Baumann et al. (2010).”
Accurate fundamental parameters for lower main‐sequence stars (2006, background): “However, abundance analysis for latetype dwarfs can still be troublesome in some cases (e.g. Allende Prieto et al. 2004).”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “For reference, a typical value for dwarfs and subgiants is around 1 − 1.5 km s−1, going up to 2 − 2.5 km s−1 for stars on the red-giant branch (RGB), and possibly as high as 5 km s−1 in supergiants (e.g., Nissen 1981; Gray et al. 2001; Allende Prieto et al. 2004; Roederer & Sneden 2011).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, result): “…(2001), Taylor & Croxall (2005), Luck & Heiter (2006) and Fuhrmann (2008), but in contrast with other studies, which rather favour a peak in the range−0.2 to −0.1 dex (e.g., Wyse & Gilmore 1995; Rocha-Pinto & Maciel 1996; Allende Prieto et al. 2004; Nordström et al. 2004; Holmberg et al. 2007).”
Abundances of Baade’s Window Giants from Keck HIRES Spectra. I. Stellar Parameters and [Fe/H] Values (2005, methodology): “This was done using a summation of 104 Gaussian fits with ¼ 0:283 dex, each centered on the [Fe/H] value of one of the stars in the Allende Prieto et al. (2004) sample.”
Properties of planets in binary systems - The role of binary separation (2006, methodology): “The lack of peculiar abundance of neutron capture elements ([Ba/Fe]= –0.12; Allende Prieto et al. 2004) suggests an original mass for the AGB star smaller than 1.3−1.5 M (Busso et al. 1999), in agreement with our estimate of ∼1.2 M .”
Abundances in a Large Sample of Stars in M3 and M13 (2004, methodology): “G. Charbonnel, D. Schaerer, & G. Meynet (San Francisco: ASP), 275 Asplund, M., Grevesse, N., Sauval, A. J., Allende Prieto, C., & Kiselman, D. 2004, A&A, 417, 751 Asplund, M., Nordlund, A., Trampedach, R., Prieto, C. A., & Stein, R. F. 2000, A&A, 359, 729 Bard, A., & Kock, M. 1994, A&A, 282, 1014 Ba”
Lithium depletion in solar-like stars: no planet connection (2010, methodology): “HARPS spectra for 12 more stars were obtained from the ESO archive, while spectra for 6 other stars were obtained from the S4N database (Allende Prieto et al. 2004)2.”
FUNDAMENTAL PARAMETERS AND CHEMICAL COMPOSITION OF ARCTURUS (2011, methodology): “We use a classical isochrone fitting technique to determine Arcturus’ age, mass, and log g. Details of our particular implementation will be given in a forthcoming paper (Ramı́rez et al. 2011, but see also Reddy et al. 2003 and Allende Prieto et al. 2004, who use essentially the same approach).”