J/A+A/579/A20 Circumstellar debris discs (Maldonado+, 2015) Searching for signatures of planet formation in stars with circumstellar debris discs. Maldonado J., Eiroa C., Villaver E., Montesinos B., Mora A. =2015A&A...579A..20M (SIMBAD/NED BibCode) ADC_Keywords: Stars, late-type ; Planets ; Abundances Keywords: techniques: spectroscopic - stars: abundances - stars: late-type - planetary systems Abstract: Tentative correlations between the presence of dusty circumstellar debris discs and low-mass planets have recently been presented. In parallel, detailed chemical abundance studies have reported different trends between samples of planet and non-planet hosts. Whether these chemical differences are indeed related to the presence of planets is still strongly debated. We aim to test whether solar-type stars with debris discs show any chemical peculiarity that could be related to the planet formation process. We determine in a homogeneous way the metallicity, [Fe/H], and abundances of individual elements of a sample of 251 stars including stars with known debris discs, stars harbouring simultaneously debris discs and planets, stars hosting exclusively planets, and a comparison sample of stars without known discs or planets. High-resolution echelle spectra (R∼57000) from 2-3m class telescopes are used. Our methodology includes the calculation of the fundamental stellar parameters (Teff, logg, microturbulent velocity, and metallicity) by applying the iron ionisation and equilibrium conditions to several isolated Fe i and Fe ii lines, as well as individual abundances of C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn. Description: The high-resolution spectra used in this work come from several spectrographs and telescopes and have already been used in some of our previous works (Maldonado et al., 2010, Cat. J/A+A/521/A12, 2012, Cat. J/A+A/541/A40, 2013, Cat. J/A+A/554/A84; Martinez-Arnaiz et al., 2010, Cat. J/A+A/520/A79), which can be consulted for details concerning the observing runs and the reduction procedure. Summarising, the data were taken with the following instruments: i) FOCES at the 2.2-m telescope of the Calar Alto observatory (CAHA, Almeria, Spain); ii) SARG at the Telescopio Nazionale Galileo (TNG, 3.58m), La Palma (Canary Islands, Spain); iii) FIES at the Nordic Optical Telescope (NOT, 2.56m), La Palma; and iv) HERMES at the Mercator telescope (1.2m), also in La Palma. We used additional spectra from the public library "S4N" (Allende Prieto et al., 2004, Cat. J/A+A/420/183), which contains spectra taken with the 2d coude spectrograph at McDonald Observatory and the FEROS instrument at the ESO 1.52m telescope in La Silla; from the ESO/ST-ECF Science Archive Facility (http://archive.eso.org/cms/); and from the pipeline processed FEROS and HARPS data archive (http://archive.eso.org/wdb/wdb/eso/repro/form). File Summary: FileName Lrecl Records Explanations ReadMe 80 . This file table2.dat 85 252 Spectroscopic parameters with uncertainties for the stars measured in this work table11.dat 256 251 Derived abundances [X/H] See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Byte-by-byte Description of file: table2.dat Bytes Format Units Label Explanations 1 A1 --- Group [A-G] Group (1) 3- 8 I6 --- HIP HIP number (0 for Sun) 9 A1 --- n_HIP [x*] Note on HIP (2) 11- 16 I6 --- HD ? HD number 18- 21 I4 K Teff Effective temperature 23- 25 I3 K e_Teff rms uncertainty on Teff 27- 30 F4.2 [cm/s2] logg Surface gravity 32- 35 F4.2 [cm/s2] e_logg rms uncertainty on logg 37- 40 F4.2 km/s vt Microturbulent velocity 42- 45 F4.2 km/s e_vt rms uncertainty on vt 47- 51 F5.2 [-] [Fe/H] Metallicity 53- 56 F4.2 [-] e_[Fe/H] rms uncertainty on [Fe/H] 58- 61 F4.2 [-] Mean iron abundance derived from FeI lines 63- 66 F4.2 [-] e_ rms uncertainty on 68- 70 I3 --- NFeI Number of FeI lines used 72- 75 F4.2 [-] Mean iron abundance derived from FeII lines 77- 80 F4.2 [-] e_ rms uncertainty on 82- 83 I2 --- NFeII Number of FeI lines used 85 A1 --- Spect Spectrograph (3) Note (1): Groups as follows: A = Stars with known debris discs B = Stars without known debris discs C = Stars with debris discs and planets D = Giant stars with debris discs and planets E = Stars with known cool Jupiters F = Stars with known low-mass planets G = Stars with hot Jupiters Note (2): Notes as follows: x = It also hosts cool- and hot-Jupiter planets * = It also hosts cool-Jupiter planets Note (3): Spectrograph as follows: 1 = CAHA/FOCES 2 = TNG/SARG 3 = NOT/FIES 4 = Mercator/HERMES 5 = S4N-McD 6 = S4N-FEROS 7 = ESO/FEROS 8 = ESO/HARPS Byte-by-byte Description of file: table11.dat Bytes Format Units Label Explanations 1- 6 I6 --- HIP HIP number 7 A1 --- n_HIP [*x] Note on HIP (1) 9- 16 A8 --- Sample Sample (2) 17 A1 --- n_Sample [+] Note on Sample (1) 19- 23 F5.2 [-] CI ?=- CI abundance ([CI/H]) 25- 29 F5.2 [-] OI ?=- OI abundance ([OI/H]) 31- 35 F5.2 [-] NaI ?=- NaI abundance ([NaI/H]) 37- 41 F5.2 [-] MgI ?=- MgI abundance ([MgI/H]) 43- 47 F5.2 [-] AlI ?=- AlI abundance ([AlI/H]) 49- 53 F5.2 [-] SiI ?=- SiI abundance ([SiI/H]) 55- 59 F5.2 [-] SI ?=- SI abundance ([SI/H]) 61- 65 F5.2 [-] CaI ?=- CaI abundance ([CaI/H]) 67- 71 F5.2 [-] ScI ?=- ScI abundance ([ScI/H]) 73- 77 F5.2 [-] ScII ?=- ScII abundance ([ScII/H]) 79- 83 F5.2 [-] TiI ?=- TiI abundance ([TiI/H]) 85- 89 F5.2 [-] TiII ?=- TiII abundance ([TiII/H]) 91- 95 F5.2 [-] VI ?=- VI abundance ([VI/H]) 97-101 F5.2 [-] CrI ?=- CrI abundance ([CrI/H]) 103-107 F5.2 [-] CrII ?=- CrII abundance ([CrII/H]) 109-113 F5.2 [-] MnI ?=- MnI abundance ([MnI/H]) 115-119 F5.2 [-] CoI ?=- CoI abundance ([CoI/H]) 121-125 F5.2 [-] NiI ?=- NiI abundance ([NiI/H]) 127-131 F5.2 [-] CuI ?=- CuI abundance ([CuI/H]) 133-137 F5.2 [-] ZnI ?=- ZnI abundance ([ZnI/H]) 139-142 F4.2 [-] e_CI ?=- rms uncertainty on CI abundance 145-148 F4.2 [-] e_OI ?=- rms uncertainty on OI abundance 151-154 F4.2 [-] e_NaI ?=- rms uncertainty on NaI abundance 157-160 F4.2 [-] e_MgI ?=- rms uncertainty on MgI abundance 163-166 F4.2 [-] e_AlI ?=- rms uncertainty on AlI abundance 169-172 F4.2 [-] e_SiI ?=- rms uncertainty on SiI abundance 175-178 F4.2 [-] e_SI ?=- rms uncertainty on SI abundance 181-184 F4.2 [-] e_CaI ?=- rms uncertainty on CaI abundance 187-190 F4.2 [-] e_ScI ?=- rms uncertainty on ScI abundance 193-196 F4.2 [-] e_ScII ?=- rms uncertainty on ScII abundance 199-202 F4.2 [-] e_TiI ?=- rms uncertainty on TiI abundance 205-208 F4.2 [-] e_TiII ?=- rms uncertainty on TiII abundance 211-214 F4.2 [-] e_VI ?=- rms uncertainty on VI abundance 217-220 F4.2 [-] e_CrI ?=- rms uncertainty on CrI abundance 223-226 F4.2 [-] e_CrII ?=- rms uncertainty on CrII abundance 229-232 F4.2 [-] e_MnI ?=- rms uncertainty on MnI abundance 235-238 F4.2 [-] e_CoI ?=- rms uncertainty on CoI abundance 241-244 F4.2 [-] e_NiI ?=- rms uncertainty on NiI abundance 247-250 F4.2 [-] e_CuI ?=- rms uncertainty on CuI abundance 253-256 F4.2 [-] e_ZnI ?=- rms uncertainty on ZnI abundance Note (1): Notes as follows: x = It also hosts cool and hot-Jupiter planets * = It also hosts cool-Jupiter planets + = Giant star Note (2): Samples as follows: SWDs = stars with discs SWODs = stars without known discs SWDPs = stars harbouring simultaneously debris discs and planets Cool = stars hosting cool (a>0.1AU) gas-giant planets Hot = stars hosting at least one close-in (a<0.1AU) gas-giant Low-mass = stars hosting at least one low-mass (Mpsini≲30M{earth}) planet History: From electronic version of the journal (End) Patricia Vannier [CDS] 28-Sep-2015