Access to Astronomical Catalogues

← Click to display the menu
J/A+A/614/A55    Lithium abundance in dwarfs & subgiants (Aguilera-Gomez+, 2018)

Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert. Aguilera-Gomez C., Ramirez I., Chaname J. <Astron. Astrophys. 614, A55 (2018)> =2018A&A...614A..55A (SIMBAD/NED BibCode)
ADC_Keywords: Abundances ; Stars, G-type ; Stars, masses ; Stars, ages ; Stars, F-type Keywords: stars: abundances - stars: evolution Abstract: We address the existence and origin of the lithium (Li) desert, a region in the Li-Teff plane sparsely populated by stars. Here we analyze some of the explanations that have been suggested for this region, including mixing in the late main sequence, a Li dip origin for stars with low Li abundances in the region, and a possible relation with the presence of planets. To study the Li desert, we measured the atmospheric parameters and Li abundance of 227 late-F dwarfs and subgiants, chosen to be in the Teff range of the desert and without previous Li abundance measurements. Subsequently, we complemented those with literature data to obtain a homogeneous catalog of 2318 stars, for which we compute masses and ages. We characterize stars surrounding the region of the Li desert. We conclude that stars with low Li abundances below the desert are more massive and more evolved than stars above the desert. Given the unexpected presence of low Li abundance stars in this effective temperature range, we concentrate on finding their origin. We conclude that these stars with low Li abundance do not evolve from stars above the desert: at a given mass, stars with low Li (i.e., below the desert) are more metal-poor. Instead, we suggest that stars below the Li desert are consistent with having evolved from the Li dip, discarding the need to invoke additional mixing to explain this feature. Thus, stars below the Li desert are not peculiar and are only distinguished from other subgiants evolved from the Li dip in that their combination of atmospheric parameters locates them in a range of effective temperatures where otherwise only high Li abundance stars would be found (i.e., stars above the desert). Description: In this work, we derive stellar parameters and lithium abundances of 227 stars. The spectra we used have high resolution (∼60000) and high signal-to-noise ratio (S/N>100), and were obtained with either the MIKE Spectrograph at Las Campanas Observatory, or with the Tull coude spectrograph on the 2.7m Harlan J. Smith Telescope at McDonald Observatory. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 52 227 Atmospheric parameters and Li abundances for the 227 stars presented in this work table3.dat 122 2318 Catalog of stellar parameters and Lithium abundances
See also: J/A+A/363/239 : Lithium abundances in single giant stars (De Medeiros+, 2000) J/A+A/371/943 : Lithium abundances for 185 main-sequence stars (Chen+, 2001) J/A+A/409/251 : Li abundances and velocities in F and G stars (Mallik+, 2003) J/A+A/538/A36 : Lithium abundances of bulge RGB stars (Lebzelter+, 2012) J/ApJ/756/46 : Lithium abundances in HIP stars (Ramirez+, 2012) J/ApJ/785/94 : Lithium abundances of a large sample of red giants (Liu+, 2014) J/A+A/595/A18 : Lithium abundances in AMBRE stars (Guiglion+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [HIP] 4- 9 I6 --- HIP HIP identifier (NNNNNN) 10 A1 --- m_HIP [AB] Multiplicity index on HIP identifier 12- 15 I4 K Teff [5686/6617] Effective temperature 17- 18 I2 K e_Teff [20/85] Uncertainty in Teff 20- 23 F4.2 [cm/s2] logg [3.5/4.5] Log of the surface gravity logg 25- 28 F4.2 [cm/s2] e_logg [0/0.12] Uncertainty in logg 30- 34 F5.2 [-] [Fe/H] [-0.34/0.36] Metallicity [Fe/H] 36- 39 F4.2 [-] e_[Fe/H] [0.03/0.16] Uncertainty in [Fe/H] 41 A1 --- l_ALi Limit flag on A(Li) 44- 47 F4.2 --- ALi [0.5/3.51] Lithium abundance A(Li) 49- 52 F4.2 --- e_ALi [0.01/0.07]? Uncertainty in A(Li)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [HIP] 4- 9 I6 --- HIP HIP identifier (NNNNNN) 10 A1 --- m_HIP [AB] Multiplicity index on HIP identifier 12- 15 I4 K Teff [4153/7165] Effective temperature 17- 19 I3 K e_Teff [50/139] Uncertainty in Teff 21- 24 F4.2 [cm/s2] logg [3.43/4.74]?=9.99 Log of the surface gravity 26- 29 F4.2 [cm/s2] e_logg [0/0.44] Uncertainty in logg 31- 35 F5.2 [-] [Fe/H] [-2.3/0.62] Metallicity 37- 40 F4.2 [-] e_[Fe/H] [0.04/0.31] Uncertainty in [Fe/H] 42 A1 --- l_ALi Limit flag on A(Li) 44- 48 F5.2 --- ALi [-1.06/3.54] Lithium abundance A(Li) 50- 53 F4.2 --- e_ALi [0/0.83]? Uncertainty in A(Li) 55- 58 F4.2 Msun Mass [0.57/1.87]?=0 Star mass 60- 63 F4.2 Msun E_Mass ?=0 Upper limit uncertainty in Mass 65- 68 F4.2 Msun e_Mass ?=0 Lower limit uncertainty in Mass 70- 74 F5.2 Gyr Age [0.1/14.9]? Star age 76- 79 F4.2 Gyr E_Age [0/9.05]? Upper limit uncertainty in Age 81- 84 F4.2 Gyr e_Age [0/9.24]? Lower limit uncertainty in Age 86- 88 A3 --- n_Age Age determination method: iso=isochrones, rot=rotation. 90- 92 A3 --- Pl [yes/no]? Known planet-host? 94-122 A29 --- Source References (1)
Note (1): References as follows: R12 = Ramirez et al., 2012, Cat. J/ApJ/756/46 B10 = Baumann et al., 2010, Cat. J/A+A/519/A87 G10 = Gonzalez et al., 2010, Cat. J/MNRAS/403/1368 I09 = Israelian et al., 2009Natur.462..189I LH06 = Luck & Heiter, 2006AJ....131.3069L T10 = Takeda et al., 2010, Cat. J/A+A/515/A93 Gh10 = Ghezzi et al., 2010, Cat. J/ApJ/724/154 LR04 = Lambert & Reddy, 2004, Cat. J/MNRAS/349/757 DM14 = Delgado Mena et al., 2014, Cat. J/A+A/562/A92 DM15 = Delgado Mena et al., 2015, Cat. J/A+A/576/A69 G1415 = Gonzalez, 2014MNRAS.441.1201G and Gonzalez, 2015, Cat. J/MNRAS/446/1020 This = This Work
Acknowledgements: Claudia Aguilera Gomez, caguiler(at)astro.puc.cl
(End) Patricia Vannier [CDS] 15-Mar-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Université de Strasbourg/CNRS

    • Contact