J/A+A/634/A34 Complete line list and solar values (Baratella+, 2020)
The Gaia-ESO Survey: a new approach to chemically characterising
young open clusters.
Baratella M., D'Orazi V., Carraro G., Desidera S., Randich S., Magrini L.
Adibekyan V., Smiljanic R., Spina L., Tsantaki M., Tautvaisiene G.,
Sousa S.G., Jofre P., Jimenez-Esteban F.M., Delgado-Mena E., Martell S.,
Van der Swaelmen M., Roccatagliata V., Gilmore G., Alfaro E.J., Bayo A.,
Bensby T., Bragaglia A., Franciosini E., Gonneau A., Heiter U.,
Hourihane A., Jeffries R.D., Koposov S.E., Morbidelli L., Prisinzano L.,
Sacco G., Sbordone L., Worley C., Zaggia S., Lewis J.
<Astron. Astrophys. 634, A34 (2020)>
=2020A&A...634A..34B 2020A&A...634A..34B (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, G-type ; Atomic physics
Keywords: stars: abundances - stars: fundamental parameters -
stars: solar-type - open clusters and associations: individual:
IC 2391, IC 2602, IC 4665, NGC 2264, NGC 2516, NGC 2547
Abstract:
Open clusters are recognised as excellent tracers of the Galactic thin
disc properties. At variance with intermediate-age and old open
clusters, for which a conspicuous number of studies is now available,
until a few years ago clusters younger than 150Myr had been mostly
overlooked in terms of their chemical composition (with few
exceptions). On the other hand, previous investigations seem to
indicate an anomalous behaviour of young clusters, which include (but
is not limited to) slightly sub-solar iron (Fe) abundances and
extreme, unexpected barium (Ba) enhancements. In a series of papers,
we plan to expand our comprehension of this topic and investigate
whether these chemical peculiarities are instead related to abundance
analysis techniques. We present here a new determination of the
atmospheric parameters for 23 dwarf stars observed by the Gaia-ESO
survey in five young open clusters (age less than 150Myr) and one
star forming region (NGC 2264). We exploit a new method based on
titanium (Ti) lines to derive spectroscopic surface gravity and, most
important, microturbulence parameter. A combination of Ti and Fe lines
have been used to obtain effective temperatures. We also infer
abundances of FeI, FeII, TiI, TiII, NaI, MgI, AlI, SiI, CaI, CrI and
NiI. Our findings are in fair agreement with Gaia-ESO iDR5 results for
effective temperatures and surface gravities, but suggest that for
very young stars the microturbulence parameter is over-estimated when
Fe lines are employed. This impacts the derived chemical composition,
causing the metal content of very young clusters to be
under-estimated. Our clusters display a metallicity [Fe/H] between
+0.04 and +0.12; thus they are not more metal-poor than the Sun.
Although based on a relatively small sample size, our explorative
study suggests that we may not need to call for ad hoc explanations to
reconcile the chemical composition of young open clusters with
Galactic chemical evolution models.
Description:
Line list used in this study (table2.dat), complete of the atomic
data, references of the log(gf) values adopted and with equivalent
width and abundances measured in the Sun.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 75 229 Complete line list
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Element Element symbol (e.g. Fe)
4- 5 A2 --- Ion [I II] Ionisation stage (1)
12- 19 F8.3 0.1nm lambda Wavelenght
23- 27 F5.3 eV EP Excitation potential
31- 36 F6.3 [-] loggf Adopted log(gf) values
40- 58 A19 --- r_loggf Reference code for log(gf) values (2)
62- 67 F6.2 0.1pm EWsun Equivalent width measured in the Sun
71- 75 F5.3 --- log(X)sun Solar abundances (3)
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Note (1): Ionisation stage as follows:
I = neutral
II = singly ionised
Note (2): Reference codes for the log(gf) values correspond to the following
references:
GESMCHF = Froese Fischer & Tachiev (2012, Multiconfiguration
Hartree-Fock and Multiconfiguration Dirac-Hartree-Fock
Collection, Version 2, http://physics.nist.gov/mchf/)
1990JQSRT..43..207C 1990JQSRT..43..207C = Chang & Tang (1990JQSRT..43..207C 1990JQSRT..43..207C)
1993JPhB...26.4409B 1993JPhB...26.4409B = Butler et al. (1993JPhB...26.4409B 1993JPhB...26.4409B)
1995JPhB...28.3485M 1995JPhB...28.3485M = Mendoza et al. (1995JPhB...28.3485M 1995JPhB...28.3485M)
GARZ = Garz (1973A&A....26..471G 1973A&A....26..471G)
BL = O'Brian & Lawler (1991, Phys. rev. A, 44, 7134)
K07 = Kurucz (2007, on-line database of observed and
predicted atomic transitions,
http://kurucz.harvard.edu/atoms)
1993PhyS...48..297N 1993PhyS...48..297N = Nahar (1993, Phys. Src. 48, 297)
SR = Smith & Raggett
(1981, J. Phys. B: At. Mol. Phys., 14, 4015)
DIKH = Drozdowski et al. (1997, Zeitschrift fur Physik D
Atoms Molecules Clusters, 41, 125 )
LGWSC = Lawler et al. (2013ApJS..205...11L 2013ApJS..205...11L)
2013ApJS..205...11L 2013ApJS..205...11L = Lawler et al. (2013ApJS..205...11L 2013ApJS..205...11L)
MFWi = Martin et al. (1988, Cat. VI/72)
2013ApJS..208...27W 2013ApJS..208...27W = Wood et al. (2013ApJS..208...27W 2013ApJS..208...27W)
SLS = Sobeck et al. (007, Cat. J/ApJ/667/1267)
GESHRL14 = Den Hartog et al. (2014, 2014arXiv1409.8142D 2014arXiv1409.8142D)
BKK = Bard et al. (1991A&A...248..315B 1991A&A...248..315B)
GESB79b = Blackwell et al. (1979MNRAS.186..657B 1979MNRAS.186..657B)
BWL = O'Brian et al. (1991, Journal of the Optical Society
of America B Optical Physics, 8, 1185
GESB82c = Blackwell et al. (1982MNRAS.199...21B 1982MNRAS.199...21B)
BIPS = Blacwell, Ibbetson et al. (1979MNRAS.186..633B 1979MNRAS.186..633B)
MRW = May et al. (1974A&AS...18..405M 1974A&AS...18..405M)
2014MNRAS.441.3127R 2014MNRAS.441.3127R = Ruffoni et al. (2014MNRAS.441.3127R 2014MNRAS.441.3127R)
GESB82d = Blackwell, Petford & Simmons (1982MNRAS.201..595B 1982MNRAS.201..595B)
GESB86 = Blackwell et al. (1986MNRAS.220..289B 1986MNRAS.220..289B)
RU = Raassen & Uylings (1998, Cat. J/A+A/340/300)
2009AA...497..611M = Melendez & Barbuy (2009A&A...497..611M 2009A&A...497..611M)
2003ApJ...584L.107J 2003ApJ...584L.107J = Johansson et al. (2003ApJ...584L.107J 2003ApJ...584L.107J)
2014ApJS..211...20W 2014ApJS..211...20W = Wood et al. (2014ApJS..211...20W 2014ApJS..211...20W)
K08 = Kurucz (2008, on-line database of observed and
predicted atomic transitions,
http://kurucz.harvard.edu/atoms) )
LWST = Lennard et al. (1975ApJ...197..517L 1975ApJ...197..517L)
If the reference code contains +, the adopted log(gf) values are the average
from more sources, while if the code contains ",", it means that the
gf-value is taken from the first source but then re-normalised to an
absolute scale using accurate lifetime measurements from the second source.
Note (3): Solar abundances computed with the following atmospheric parameters:
Teff/logg/xi=5790/4.47/1.00
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Acknowledgements:
Martina Baratella, martina.baratella.1(at)phd.unipd.it
(End) Martina Baratella [UniPD], Patricia Vannier [CDS] 10-Jan-2020