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.
<Astron. Astrophys., 579, A20-20 (2015)>
=2015A&A...579A..20M 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:
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FileName Lrecl Records Explanations
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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]
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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 [-] <A(FeI)> Mean iron abundance derived from FeI lines
63- 66 F4.2 [-] e_<A(FeI)> rms uncertainty on <A(FeI)>
68- 70 I3 --- NFeI Number of FeI lines used
72- 75 F4.2 [-] <A(FeII)> Mean iron abundance derived from FeII lines
77- 80 F4.2 [-] e_<A(FeII)> rms uncertainty on <A(FeII)>
82- 83 I2 --- NFeII Number of FeI lines used
85 A1 --- Spect Spectrograph (3)
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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
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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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
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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
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 28-Sep-2015