J/A+A/664/A70 Lithium depletion boundary in stellar assoc. (Galindo-Guil+, 2022)
Lithium depletion boundary, stellar associations and Gaia.
Galindo-Guil F.J., Barrado D., Bouy H., Olivares J., Bayo A.,
Morales-Calderon M., Huelamo N., Sarro L. M., Riviere-Marichalar P.,
Stoev H., Montesinos B., Stauffer J.R.
<Astron. Astrophys. 664, A70 (2022)>
=2022A&A...664A..70G 2022A&A...664A..70G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, brown dwarf ; Equivalent widths ; Optical
Keywords: open clusters and associations: general - stars: brown dwarfs -
stars: fundamental parameters - stars: low-mass stars
Abstract:
Stellar ages are key to improving our understanding of different
astrophysical phenomena. However, many techniques to estimate stellar
ages are highly model-dependent. The lithium depletion boundary (LDB),
based on the presence or absence of lithium in low-mass stars, can be
used to derive ages in stellar associations of between 20 and 500Ma.
The purpose of this work is to revise former LDB ages in stellar
associations in a consistent way, taking advantage of the homogeneous
Gaia parallaxes as well as bolometric luminosity estimations that do
not rely on monochromatic bolometric corrections.
We studied nine open clusters and three moving groups characterised by
a previous determination of the LDB age. We gathered all the available
information from our data and the literature: membership, distances,
photometric data, reddening, metallicity, and surface gravity. We
re-assigned membership and calculated bolometric luminosities and
effective temperatures using distances derived from Gaia DR2 and
multi-wavelength photometry for individual objects around the former
LDB. We located the LDB using a homogeneous method for all the stellar
associations. Finally, we estimated the age by comparing it with
different evolutionary models.
We located the LDB for the twelve stellar associations and derived
their ages using several theoretical evolutionary models. We compared
the LDB ages among them, along with data obtained with other
techniques, such as isochrone fitting, ultimately finding some
discrepancies among the various approaches. Finally, we remark that
the 32 Ori MG is likely to be composed of at least two populations of
different ages.
Description:
Table E.4., includes calculated and collected stellar parameters for
each object from each LDB sample.
Parallaxes and proper motions were taken from Gaia DR2.
(rho) is the correlation between proper motion in right ascension and
proper motion in declination.
(EWLi) is the equivalent width of lithium at 6707.8Å, with its
reference. Equivalent width of a lithium-poor object is given by an
upper limit or without any measure.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablee4.dat 218 578 Stellar properties and astrometric data from
Gaia DR2 for all LDB samples
--------------------------------------------------------------------------------
See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
Byte-by-byte Description of file: tablee4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Object Name of the object
18 I1 --- n_Object [1/6]? Note on object (1)
20- 31 A12 --- Assoc Name of the stellar association
33- 43 F11.7 deg RAdeg Right ascension (J2000.0)
45- 55 F11.7 deg DEdeg Declination (J2000.0)
57- 63 F7.3 mas plx ? Parallax (parallax) from Gaia DR2
65- 69 F5.3 mas e_plx ? Standard error of parallax (parallax_error)
from Gaia DR2
71- 78 F8.3 mas/yr pmRA ? Proper motion in right ascension direction,
pmRA*cosDE (pmra) from Gaia DR2
80- 84 F5.3 mas/yr e_pmRA ? Error in proper motion in right ascension
direction, (e_pmra) from Gaia DR2
86- 93 F8.3 mas/yr pmDE ? Proper motion in declination direction,
(pmdec) from Gaia DR2
95- 99 F5.3 mas/yr e_pmDE ? Error in proper motion in declination
direction, (e_pmdec) from Gaia DR2
101-106 F6.3 --- rho [-1/1]? Correlation between proper motion in
right ascension and proper motion in
declination (pmrapmdeccorr) from Gaia DR2
108-110 A3 --- l_EWLi [≤Y?-. ] Limit flag on EWLi (2)
112-118 F7.4 0.1nm EWLi ? Lithium equivalent width or lower value of
lithium equivalent width interval
119 A1 --- --- [-]
120-124 F5.3 0.1nm EWLimax ? Upper value of lithium equivalent width
interval
125-130 F6.4 0.1nm E_EWLi ? Uncertainty based on the inter-68th
percentile range, 1σ error,
positive uncertainty (3)
132-137 F6.4 0.1nm e_EWLi ? Uncertainty based on the inter-68th
percentile range, 1σ error,
positive uncertainty (3)
139-140 I2 --- r_EWLi ? Reference for the Lithium equivalent width
assumed (4)
142 A1 --- Lirich [Y?N] Lithium richness of the object (5)
144-158 A15 --- Remarks Remarks of the object (6)
160-166 F7.2 pc dmap ?=- Most likely distance (dMAP) (7)
168-174 F7.2 pc b_dmap ?=- 2.5th percentile distance confidence
interval (d025) (7)
176-182 F7.2 pc B_dmap ?=- 97.5th percentile distance confidence
interval (d975) (7)
184-187 I4 K TeffChi Effective temperature with mininimization of
Chi2 (8)
189-197 F9.3 Lsun LBol Most likely bolometric luminosity (LBolMAP)
199-208 F10.4 Lsun LBolmin 2.5th percentile bolometric luminosity
confidence interval (d025)
210-218 F9.3 Lsun LBolmax 97.5th percentile bolometric luminosity
confidence interval (d975)
--------------------------------------------------------------------------------
Note (1): Note on object as follows:
1 = Undetermined lithium detection, see Section 5.9.
2 = Negative LBolmin value. The uncertainty in Ftot is bigger than Ftot,
see Section 4.3.
3 = The next sources are binary systems only resolved in Gaia DR2:
01132817a and 01132817a, 01535076a and 01535076b, and 02335984a
and 02335984b.
4 = THOR-14Aa and THOR-14Ab are two sources resolved in Gaia DR2, but in the
rest of photometric surveys considered are blended.
5 = J05053333 is the short name of 2MASS J05053333+0044034.
6 = Peculiar objects described in Appendix C.
Note (2): Limit flag on lithium equivalent width as follows:
< = Equivalent width upper limit of a lithium-poor object
(notation depends on the previous work).
≤ = Equivalent width upper limit of a lithium-poor object
(notation depends on the previous work).
- = Lithium-poor object without any measure.
Y = Lithium-rich object without any measure, see Manzi et al.
(2008A&A...479...141M, Cat. J/A+A/479/141)
Y? = Lithium-rich object without any measure, see Manzi et al.
(2008A&A...479...141M, Cat. J/A+A/479/141)
... = Undetermined lithium content because of low resolving power, low
signal-to-noise ratio, bad quality, or it does not cover this part
of the spectrum.
Note (3): E_EWLi and e_EWLi are the EWLi standard deviation.
The exception is some Blanco_1 objects.
In that case, the EWLi we report are determined from the mode of the
marginalized distribution with uncertainties based on the inter-68th
percentile range, 1σ errors, (E_EWLi) and (e_EWLi),
see Juarez et al. (2014ApJ...795...143J).
Note (4): References for lithium equivalent width as follows:
1 = Stauffer et al. (1999ApJ...527..219S 1999ApJ...527..219S)
2 = Basri et al. (1999ApJ...510..266B 1999ApJ...510..266B)
3 = Zapatero Osorio et al. (1996A&A...305..519Z 1996A&A...305..519Z)
4 = Jeffries et al. (2013MNRAS.434.2438J 2013MNRAS.434.2438J, Cat. J/MNRAS/434/2438)
5 = Manzi et al. (2008A&A...479..141M 2008A&A...479..141M, Cat. J/A+A/479/141)
6 = Jeffries et al. (2009MNRAS.400..317J 2009MNRAS.400..317J, Cat. J/MNRAS/400/317)
7 = Jeffries et al. (2005MNRAS.358...13J 2005MNRAS.358...13J)
8 = Dobbie et al. (2010MNRAS.409.1002D 2010MNRAS.409.1002D)
9 = Barrado et al. (2004ApJ...614..386B 2004ApJ...614..386B)
10 = Boudreault et al. (2009ApJ...706.1484B 2009ApJ...706.1484B, Cat. J/ApJ/706/1484)
11 = Marcy et al. (1994ApJ...428L..57M 1994ApJ...428L..57M)
12 = Basri et al. (1996ApJ...458..600B 1996ApJ...458..600B)
13 = Rebolo et al. (1996ApJ...469L..53R 1996ApJ...469L..53R)
14 = Oppenheimer et al. (1997AJ....113..296O 1997AJ....113..296O)
15 = Stauffer et al. (1998ApJ...499L.199S 1998ApJ...499L.199S)
16 = Stauffer et al. (1998ApJ...504..805S 1998ApJ...504..805S)
17 = Martin et al. (1998ApJ...507L..41M 1998ApJ...507L..41M)
18 = Martin et al. (2000ApJ...543..299M 2000ApJ...543..299M)
19 = Dahm et al. (2015ApJ...813..108D 2015ApJ...813..108D)
20 = Cargile et al. (2010ApJ...725.1111I 2010ApJ...725.1111I)
21 = Juarez et al. (2014ApJ...795..143J 2014ApJ...795..143J)
22 = Martin et al. (2018ApJ...856...40M 2018ApJ...856...40M)
23 = Lodieu et al. (2018A&A...615L..12L 2018A&A...615L..12L, Cat. J/A+A/615/L12)
24 = Reid et al. (2002AJ....124..519R 2002AJ....124..519R)
25 = Song et al. (2003ApJ...599..342S 2003ApJ...599..342S)
26 = Torres et al. (2006A&A...460..695T 2006A&A...460..695T, Cat. J/A+A/460/695)
27 = da Silva et al. (2009A&A...508..833D 2009A&A...508..833D, Cat. J/A+A/508/833)
28 = Kiss et al. (2011MNRAS.411.1177P 2011MNRAS.411.1177P)
29 = Moor et al. (2013MNRAS.435.1376M 2013MNRAS.435.1376M)
30 = Binks et al. (2014MNRAS.438.1191S 2014MNRAS.438.1191S)
31 = Kraus et al. (2014AJ....147..146K 2014AJ....147..146K, Cat. J/AJ/147/146)
32 = Malo et al. (2014ApJ...792...37M 2014ApJ...792...37M)
33 = Rodriguez et al. (2014A&A...567A..20R 2014A&A...567A..20R)
34 = Binks et al. (2016MNRAS.455.3345B 2016MNRAS.455.3345B)
35 = Shkolnik et al. (2017AJ....154...69S 2017AJ....154...69S, cat. J/AJ/154/69)
36 = Malo et al. (2013ApJ...762...88M 2013ApJ...762...88M, Cat. J/ApJ/762/88)
37 = Bell et al. (2017MNRAS.468.1198B 2017MNRAS.468.1198B)
Note (5): The label Lirich indicates whether it is a lithium-rich or
lithium-poor object based on its lithium equivalent width (EWLi) and
previous works, listed in Note (2).
Flag as follows:
Y = Lithium-rich object
N = Lithium-poor object
? = An object with undetermined lithium content
Note (6): Remarks of the objects as follows:
CMS = Confirmed binary or multiple system.
CP = Contaminated photometry.
EL = Strong emission line object.
F = Flaring object.
FR = Fast rotator.
NM = No-member, based on this work.
P1 = Subsample with plx<9.52mas. Only for the 32OriMG sources.
P2 = Subsample with plx>9.52mas. Only for the 32OriMG sources.
RV = Radial velocity members within the range of 2 to +10km/s in 1σ,
see Figure 4 from Juarez et al. (2014ApJ...795..143J 2014ApJ...795..143J).
Only for the Blanco_1 objects.
SuB = Suspected binary or multiple system.
Note (7): If an object lacks a parallax in Gaia DR2 (plx) or it has a negative
parallax, we indicated the distances (dmap, dmin, dmax) with '---'.
Note (8): Effective temperature after fitting Teff and chi2 and minimizing this
last value, see for clarifying Barrado et al. (2016A&A...596A.113B 2016A&A...596A.113B,
Cat. J/A+A/596/A113).
--------------------------------------------------------------------------------
Acknowledgements:
F.J. Galindo-Guil, pgalindo(at)cefca.es
(End) Patricia Vannier [CDS] 20-Jun-2022