J/MNRAS/513/5727 Lithium study with GESiDR6's PMS stars cluster (Binks+, 2022)
The Gaia-ESO survey constraining evolutionary models and ages for young low
mass stars with measurements of lithium depletion and rotation.
Binks A.S., Jeffries R.D., Sacco G.G., Jackson R.J., Cao L., Bayo A.,
Bergemann M., Bonito R., Gilmore G., Gonneau A., Jiminez-Esteban F.,
Morbidelli L., Randich S., Roccatagliata V., Smiljanic R., Zaggia S.
<Mon. Not. R. Astron. Soc. 513, 5727-5751 (2022)>
=2022MNRAS.513.5727B 2022MNRAS.513.5727B (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Stars, M-type ; Stars, K-type ;
Stars, pre-main sequence ; Photometry ; Spectroscopy ; Optical ;
Infrared ; Spectral types ; Equivalent widths ; Stars, masses ;
Rotational velocities ; Effective temperatures
Keywords: stars: kinematics and dynamics - stars: late-type -
stars: pre-main-sequence - (Galaxy:) solar neighbourhood
Abstract:
A growing disquiet has emerged in recent years that standard stellar
models are at odds with observations of the colour-magnitude diagrams
(CMDs) and lithium depletion patterns of pre-main sequence stars in
clusters. In this work we select 1246 high probability K/M-type
constituent members of five young open clusters (5-125 Myr) in the
Gaia-ESO Survey to test a series of models that use standard input
physics and others that incorporate surface magnetic fields or cool
starspots. We find that: standard models provide systematically under-
luminous isochrones for low-mass stars in the CMD and fail to predict
Li- depletion of the right strength at the right colour; magnetic
models provide better CMD fits with isochrones that are ∼1.5-2 times
older, and provide better matches to Li depletion patterns. We
investigate how rotation periods, most of which are determined here
for the first time from Transiting Exoplanet Survey Satellite data,
correlate with CMD position and Li. Among the K-stars in the older
clusters we find the brightest and least Li-depleted are the fastest
rotators, demonstrating the classic 'Li-rotation connection' for the
first time at ∼35 Myr in NGC 2547, and finding some evidence that it
exists in the early M-stars of NGC 2264 at < 10 Myr. However, the wide
dispersion in Li depletion observed in fully convective M-dwarfs in
the γ Vel cluster at ∼20 Myr appears not to be correlated with
rotation and is challenging to explain without a very large (>10 Myr)
age spread.
Description:
We study of pre-main sequence stars (PMS) Li depletion in order to
explore the extent to which various models predict their Li depletion
patterns and colour-magnitude diagrams (CMDs). To do this, we exploit
data from the Gaia-ESO Survey (GES; Gilmore et al.
2012Msngr.147...25G 2012Msngr.147...25G; Randich et al. 2013Msngr.154...47R 2013Msngr.154...47R), a large
spectroscopic programme carried out at the VLT which obtained many
thousands of spectra for stars in open clusters, measuring equivalent
widths for the Li 670.8 nm diagnostic feature (EW(Li), calculated
independently in this work using GES spectra) and radial velocities.
Similarly to the GES-based studies of Jeffries et al.
(2017MNRAS.464.1456J 2017MNRAS.464.1456J) and Franciosini et al. (2022A&A...659A..85F 2022A&A...659A..85F,
Cat. J/A+A/659/A85), who both found that models incorporating
starspots provided a better match to the CMDs and Li depletion
patterns in young clusters. Our independent study to test evolutionary
models with open clusters, using similar GES data, but incorporating a
consideration of how stellar rotation affects the observed CMD and
Li-depletion patterns. Here we focus on lower mass PMS stars (≤ 0.6
M☉) and, by combining GES spectroscopy, Gaia photometry and new
rotation periods obtained from analysis of data from the Transiting
Exoplanet Survey Satellite (TESS; Ricker et al. 2015JATIS...1a4003R 2015JATIS...1a4003R)
and other published sources, for the first time we explore whether the
connection between rotation and Li depletion is present among late-K
and M-type PMS stars prior to their total Li depletion, (i.e taken
from Introduction section).
As explained in the section 2, we proceed to selecting target in five
interesting clusters (NGC 2264, λ Ori, γ Vel, NGC 2547,
and NGC 2516) observed during the GES campaign. We select target via
high membership probabilities P3D > 0.95 (Jackson et al.
2022MNRAS.509.1664J 2022MNRAS.509.1664J, Cat. J/MNRAS/509/1664 based on GaiaEDR3
astrometric data) and good photometry, also logg > 3.0. In our
sample, all spectroscopic measurements and stellar parameters were
taken from the sixth GES internal data release. The sample contains
1248 M/K stars cluster with low M* as presented in the table2.dat.
More, as the appendix B details it, we expose measuring rotation
periods from TESS data and literature used for our analysis in the
tableb2.dat for all the stars sample.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
cluster.dat 11 5 Clusters in our sample
table2.dat 170 1246 Our stars cluster selected sample
tableb2.dat 77 1246 TESS and literature rotation periods and
the final adopted rotation period to be used
for analysis
--------------------------------------------------------------------------------
See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
J/A+A/659/A85 : Membership and lithium of young clusters (Franciosini+,2022)
J/MNRAS/509/1664 : Membership study of 70 stars clusters (Jackson+, 2022)
J/MNRAS/430/1433 : NGC 2264 members periods with CoRoT (Affer+, 2013)
J/A+A/641/A51 : NGC 2516 membership list (Fritzewski+, 2020)
J/MNRAS/377/741 : VIc photometry of NGC 2516 (Irwin+, 2007)
J/MNRAS/384/675 : Monitoring low-mass stars in NGC 2362 (Irwin+ 2008)
J/A+A/417/557 : Rotation & variability of PMS Stars in NGC 2264 (Lamm, 2004)
J/AJ/127/2228 : VRI photometry of PMS stars in NGC 2264 OB (Makidon+, 2004)
J/A+A/599/A23 : Accretion-rotation connection in NGC 2264 (Venuti+, 2017)
Byte-by-byte Description of file: cluster.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Cluster name (Cluster)
9- 11 I3 --- Nbr Number of stars in the cluster
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR2 Gaia DR2 source identifier (source_id)
21- 27 A7 --- Cluster Cluster name (Cluster)
29- 34 F6.4 --- P3D 3D kinematic membership probabilities P3D
(MEM3D)
36- 42 F7.4 mag Gmag G apparent magnitude (Vega) de-reddened
photometric from GaiaDR2 (Gmag)
44- 49 F6.4 mag e_Gmag Mean error of Gmag (eGmag)
51- 56 F6.3 mag Ksmag 2MASS Ks apparent mangitude infrared at
2.159 µm (Vega) de-reddened photometry
(Ksmag)
58- 62 F5.3 mag e_Ksmag Mean error of Ksmag (eKsmag)
64- 67 A4 --- SpType Spectral type for K and M stars (SpT)
69- 72 I4 10-4nm EW(Li) ?=-999 Li 670.8 nm equivalent width
measurements derived from our independent
analysis of GESiDR6 spectra see section 2.4
Li equivalent widths (EWLi)
74- 77 I4 10-4nm e_EW(Li) ?=-999 Mean error of EW (Li) (eEWLi)
79- 86 F8.3 0.1nm EW(Ha) ?=-999 Chromospheric Hα 656.281 nm
equivalent widths EW(HαCHR) from
the GESiDR6 (Ha10)
88- 95 F8.3 0.1nm e_EW(Ha) ?=-999 Mean error of EW (Ha) (eHa10)
97- 102 F6.1 km/s Vsini ?=-999 Projected rotational velocities
(vsini)
104- 109 F6.1 km/s e_Vsini ?=-999 Mean error of Vsini (evsini)
111- 115 F5.3 Msun M*0 0th percentile of M* (mass_00)
117- 121 F5.3 Msun M*40 40th percentile of M* (mass_40)
123- 127 F5.3 Msun M*60 60th percentile of M* (mass_60)
129- 133 F5.3 Msun M*80 80th percentile of M* (mass_80)
135- 139 F5.3 [K] logTeff0 Logarithm of 0th percentile of Teff
(logTeff_00)
141- 145 F5.3 [K] logTeff40 Logarithm of 40th percentile of Teff
(logTeff_40)
147- 151 F5.3 [K] logTeff60 Logarithm of 60th percentile of Teff
(logTeff_60)
153- 157 F5.3 [K] logTeff80 Logarithm of 80th percentile of Teff
(logTeff_80)
159- 164 F6.3 mag G0mag 0th percentile of Gmag (Gmag0)
166- 170 F5.3 mag Ks0mag 0th percentile of Ksmag (Ksmag0)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Cluster name (Cluster)
9- 27 I19 --- GaiaDR2 Gaia DR2 source identifier (source_id)
29- 34 F6.4 d PTF ? The rotation period derived in the TESS
analysis appendix B (PTF)
36- 41 F6.4 d e_PTF ? Mean error of PTF (errorPTF)
43- 44 I2 --- o_PTF Number of light curves used for calculating
PTF (N)
46- 50 F5.2 d Plit ? Literature rotation period (Plit)
52- 60 A9 --- r_Plit Reference literature of Plit (refPlit) (1)
62- 68 F7.4 d Prot ? Final rotation period used for analysis
(Prot)
70- 75 F6.4 d e_Prot ? Mean error of Prot (errorProt)
77 I1 --- n_Prot Note code on rotation period Prot (C) (2)
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Note (1): For 461 rotation periods, reference literature codes of rotation
period are as follows:
A+13 = Affer et al. 2013MNRAS.430.1433A 2013MNRAS.430.1433A, Cat. J/MNRAS/430/1433,
9 sources of our sample
F+20 = Fritzewski et al. 2020A&A...641A..51F 2020A&A...641A..51F, Cat. J/A+A/641/A51,
148 sources of our sample
I+07 = Irwin et al. 2007MNRAS.377..741I 2007MNRAS.377..741I, Cat. J/MNRAS/377/741,
79 sources of our sample
I+08 = Irwin et al. 2008MNRAS.384..675I 2008MNRAS.384..675I, Cat. J/MNRAS/384/675,
62 sources of our sample
L+04 = Lamm et al. 2004A&A...417..557L 2004A&A...417..557L, Cat. J/A+A/417/557,
31 sources of our sample
M+04 = Makidon et al. 2004AJ....127.2228M 2004AJ....127.2228M, Cat. J/AJ/127/2228,
2 sources of our sample
V+17 = Venuti et al. 2017A&A...599A..23V 2017A&A...599A..23V, Cat. J/A+A/599/A23,
105 sources of our sample
Note (2): Notes on rotation period are as follows:
0 = No period data available, neither PTF or Plit,
530 sources of our sample
1 = One light curve from TESS, no Plit available,
129 sources of our sample
2 = A Plit value available, no PTF,
239 sources of our sample
3 = Both PTF and Plit are in agreement, Prot = PTF,
161 sources of our sample
4 = PTF and Plit are in disagreement, Prot = Plit,
20 sources of our sample
5 = PTF and Plit are in disagreement, Prot = PTF,
27 sources of our sample
6 = PTF ∼ 2*Plit, Prot = Plit,
14 sources of our sample
7 = Two or more light curves from PTESS and no Plit is available,
108 sources of our sample
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 13-Jan-2025