J/A+A/659/A85 Membership and lithium of young clusters (Franciosini+, 2022)
Gaia-ESO Survey: Role of magnetic activity and starspots on pre-main
sequence lithium evolution.
Franciosini E., Tognelli E., Degl'Innocenti S., Prada Moroni P.G.,
Randich S., Sacco G.G., Magrini L., Pancino E., Lanzafame A.C.,
Smiljanic R., Prisinzano L., Sanna N., Roccatagliata V., Bonito R.,
de Laverny P., Gutierrez Albarran M.L., Montes D., Jimenez-Esteban F.,
Gilmore G., Bergemann M., Carraro G., Damiani F., Gonneau A.,
Hourihane A., Morbidelli L., Worley C.C., Zaggia S.
<Astron. Astrophys. 659, A85 (2022)>
=2022A&A...659A..85F 2022A&A...659A..85F (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Abundances ; Radial velocities ;
Parallaxes, trigonometric ; Proper motions ; Photometry
Keywords: stars: abundances - stars: evolution - stars: late-type -
stars: pre-main sequence - methods: numerical
Abstract:
It is now well known that pre-main sequence models with inflated radii
should be taken into account to simultaneously reproduce the
colour-magnitude diagram and the lithium depletion pattern observed in
young open star clusters. We test a new set of pre-main sequence
models including radius inflation due to the presence of starspots or
to magnetic inhibition of convection, using five clusters observed by
the Gaia-ESO Survey, spanning the age range ∼10-100Myr where such
effects could be important. The Gaia-ESO Survey radial velocities are
combined with astrometry from Gaia EDR3 to obtain clean lists of
high-probability members for the five clusters. A Bayesian maximum
likelihood method is adopted to fit the observed cluster sequences to
theoretical predictions to derive the best model parameters and the
cluster reddening and age. Models are calculated with different values
of the mixing length parameter (αML=2.0, 1.5 and 1.0), for the
cases with no spots or with effective spot coverage βspot=0.2
and 0.4. The models are also compared with the observed lithium
depletion patterns. To reproduce the colour-magnitude diagram and the
observed lithium depletion pattern in Gamma Vel A and B and in 25 Ori
one needs to assume both a reduced convection efficiency, with
αML=1.0, and an effective surface spot coverage of about 20%.
We obtained ages of 18+1.5-4.0 Myr and 21+3.5-3.0 Myr for
Gamma Vel A and B, respectively, and 19+1.5-7.0 Myr for 25 Ori.
However, a single isochrone is not sufficient to account for the
lithium dispersion, and an increasing level of spot coverage as mass
decreases seems to be required. On the other hand, the older clusters
(NGC 2451B at 30+3.0-5.0Myr, NGC 2547 at 35+4.0-4.0Myr, and
NGC 2516 at 138+48-42Myr) are consistent with standard models,
with αML=2.0 and no spots, except at low masses: a 20% spot
coverage appears to better reproduce the sequence of M-type stars and
might explain the observed spread in lithium abundances. The quality
of Gaia-ESO data combined with Gaia allows us to gain important
insights on pre-main sequence evolution. Models including starspots
can provide a consistent explanation of the cluster sequences and
lithium abundances observed in young clusters, although a range of
starspot coverage is required to fully reproduce the data.
Description:
Tables B.1-B.6 list the properties of the high probability members of
the young open clusters analysed in the paper (25 Ori, Gamma Vel, NGC
2451B, NGC2547 and NGC2516). The members were selected combining the
spectroscopic data from the Gaia-ESO Survey and astrometry from Gaia
EDR3 (I/350). The tables include the Gaia-ESO and Gaia EDR3
identifiers, radial velocities, temperatures and lithium abundances
from Gaia-ESO, Gaia astrometry and photometry, and the derived
membership probabilities.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 180 442 High-probability members of 25 Ori
tableb2.dat 182 325 High-probability members of Gamma Vel A
tableb3.dat 182 128 High-probability members of Gamma Vel B
tableb4.dat 182 125 High-probability members of NGC2451B
tableb5.dat 182 255 High-probability members of NGC2547
tableb6.dat 182 536 High-probability members of NGC2516
--------------------------------------------------------------------------------
See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Cname Gaia-ESO identifier
18- 36 I19 --- GaiaEDR3 Gaia EDR3 identifier
38- 46 F9.6 deg RAdeg Right Ascension (ICRS) at Ep=2016.0
from Gaia EDR3
48- 55 F8.6 deg DEdeg Declination (ICRS) at Ep=2016.0
from Gaia EDR3
57- 61 F5.2 km/s RV ?=99.99 Radial velocity from Gaia-ESO
63- 66 F4.2 km/s e_RV ?=9.99 Error in RV
68- 74 F7.1 K Teff ?=99999.9 Effective temperature from Gaia-ESO
76- 80 F5.1 K e_Teff ?=999.9 Error in Teff
82 A1 --- l_ALi [<] Upper limit flag on Li abundance
84- 88 F5.2 --- ALi ?=9.99 Lithium abundance A(Li)
90- 93 F4.2 --- e_ALi ?=9.99 Error on A(Li)
95 A1 --- n_ALi [*] Note on A(Li) (1)
97-102 F6.4 mas plx ?=9.9999 Parallax from Gaia EDR3
104-109 F6.4 mas e_plx ?=9.9999 Error in Plx
111-117 F7.4 mas/yr pmRA ?=99.9999 Proper motion in RA from Gaia EDR3
119-124 F6.4 mas/yr e_pmRA ?=9.9999 Error in pmRA
126-133 F8.4 mas/yr pmDE ?=99.9999 Proper motion in DEC from Gaia EDR3
135-140 F6.4 mas/yr e_pmDE ?=9.9999 Error in pmDE
142-147 F6.3 --- RUWE ?=99.999 Renormalized Unit Weight Factor
from Gaia EDR3
149-150 I2 --- astrflg [0/1]?=-1 Flag on astrometry (2)
152-157 F6.3 mag Gmag ?=99.999 G magnitude from Gaia EDR3
159-164 F6.3 mag BPmag ?=99.999 BP magnitude from Gaia EDR3
166-171 F6.3 mag RPmag ?=99.999 RP magnitude from Gaia EDR3
173-174 I2 --- photflg [0/1]?=-1 Flag on photometry (2)
176-180 F5.3 --- Prob Membership probability
--------------------------------------------------------------------------------
Note (1): An asterisk * in this column indicates that A(Li) is likely
overestimated because of an underestimated gravity.
Note (2): A value of 1 indicates that the corresponding astrometric or
photometric data are good, 0 indicates less reliable data.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb[23456].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Cname Gaia-ESO identifier
18- 36 I19 --- GaiaEDR3 Gaia EDR3 identifier
38- 47 F10.6 deg RAdeg Right Ascension (ICRS) at Ep=2016.0
from Gaia EDR3
49- 58 F10.6 deg DEdeg Declination (ICRS) at Ep=2016.0
from Gaia EDR3
60- 64 F5.2 km/s RV ?=99.99 Radial velocity from Gaia-ESO
66- 69 F4.2 km/s e_RV ?=9.99 Error in RV
71- 77 F7.1 K Teff ?=99999.9 Effective temperature from Gaia-ESO
79- 83 F5.1 K e_Teff ?=999.9 Error in Teff
85 A1 --- l_ALi [<] Upper limit flag on Li abundance
87- 91 F5.2 --- ALi ?=9.99 Lithium abundance A(Li)
93- 96 F4.2 --- e_ALi ?=9.99 Error on A(Li)
98-103 F6.4 mas plx ?=9.9999 Parallax from Gaia EDR3
105-110 F6.4 mas e_plx ?=9.9999 Error in Plx
112-119 F8.4 mas/yr pmRA ?=99.9999 Proper motion in RA from Gaia EDR3
121-126 F6.4 mas/yr e_pmRA ?=9.9999 Error in pmRA
128-135 F8.4 mas/yr pmDE ?=99.9999 Proper motion in DEC from Gaia EDR3
137-142 F6.4 mas/yr e_pmDE ?=9.9999 Error in pmDE
144-149 F6.3 --- RUWE ?=99.999 Renormalized Unit Weight Factor
from Gaia EDR3
151-152 I2 --- astrflg [0/1]?=-1 Flag on astrometry (1)
154-159 F6.3 mag Gmag ?=99.999 G magnitude from Gaia EDR3
161-166 F6.3 mag BPmag ?=99.999 BP magnitude from Gaia EDR3
168-173 F6.3 mag RPmag ?=99.999 RP magnitude from Gaia EDR3
175-176 I2 --- photflg [0/1]?=-1 Flag on photometry (1)
178-182 F5.3 --- Prob Membership probability
--------------------------------------------------------------------------------
Note (1): A value of 1 indicates that the corresponding astrometric or
photometric data are good, 0 indicates less reliable data.
--------------------------------------------------------------------------------
Acknowledgements:
Elena Franciosini, elena.franciosini(at)inaf.it
(End) E. Franciosini [INAF/Arcetri Obs,, Italy], P. Vannier [CDS] 20-Nov-2021