J/MNRAS/500/1158 Rotation and lithium depletion of M35 dwarfs (Jeffries+, 2021)
The effects of rotation on the lithium depletion of G- and K-dwarfs in
Messier 35.
Jeffries R.D., Jackson R.J., Sun Q., Deliyannis C.P.
<Mon. Not. R. Astron. Soc., 500, 1158-1177 (2021)>
=2021MNRAS.500.1158J 2021MNRAS.500.1158J (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Stars, G-type ; Stars, K-type ;
Stars, pre-main sequence ; Abundances, peculiar ;
Photometry, UBVRI ; Photometry, infrared ; Spectra, optical
Keywords: stars: abundances - stars: activity - stars: magnetic field -
stars: pre-main-sequence - starspots
Abstract:
New fibre spectroscopy and radial velocities from the WIYN telescope
are used to measure photospheric lithium in 242 high-probability,
zero-age main-sequence F- to K-type members of the rich cluster M35.
Combining these with published rotation periods, the connection
between lithium depletion and rotation is studied in unprecedented
detail. At Teff<5500K there is a strong relationship between faster
rotation and less Li depletion, although with a dispersion larger than
measurement uncertainties. Components of photometrically identified
binary systems follow the same relationship. A correlation is also
established between faster rotation rate (or smaller Rossby number),
decreased Li depletion and larger stellar radius at a given Teff.
These results support models where star-spots and interior magnetic
fields lead to inflated radii and reduced Li depletion during the
pre-main-sequence (PMS) phase for the fastest rotators. However, the
data are also consistent with the idea that all stars suffered lower
levels of Li depletion than predicted by standard PMS models, perhaps
because of deficiencies in those models or because saturated levels of
magnetic activity suppress Li depletion equally in PMS stars of
similar Teff regardless of rotation rate, and that slower rotators
subsequently experience more mixing and post-PMS Li depletion.
Description:
Targets for fibre spectroscopy were assembled from three sources. A
total of 310 stars with 14<V<18 were identified that had periods
measured as part of the Kepler K2 campaign (Libralato et al.
2016MNRAS.456.1137L 2016MNRAS.456.1137L) and an M35 membership probability >0.2 from the
DANCe proper motion study of Bouy et al. (2015A&A...575A.120B 2015A&A...575A.120B, Cat.
J/A+A/575/A120). Many of these also had ground-based rotation periods
recorded in Meibom, Mathieu & Stassun (2009ApJ...695..679M 2009ApJ...695..679M, Cat.
J/ApJ/695/679). A further 28 stars that only had rotation periods in
Meibom et al. (2009ApJ...695..679M 2009ApJ...695..679M, Cat. J/ApJ/695/679) were added,
with similar V magnitudes and proper motion membership probabilities.
Finally, a set of lower priority targets were selected; these had no
measured periods but were likely proper motion and photometric members
of M35, with 15.5<g<18.2 (from the Bouy et al. 2015A&A...575A.120B 2015A&A...575A.120B,
Cat. J/A+A/575/A120, catalogue) and adopting V∼0.911g+0.91 as a
transformation for the purposes of target selection.
From these lists a total of 342 targets were observed; 327 with a
measured rotation period; 301 from Libralato et al.
(2016MNRAS.456.1137L 2016MNRAS.456.1137L); 172 from Meibom et al. (2016MNRAS.456.1137L 2016MNRAS.456.1137L)
(147 are in both catalogues) and 15 with no period data.
Observations were made at the WIYN 3.5-m telescope using the Hydra
multi-object fibre spectrograph (Bershady et al. 2008SPIE.7014E..0HB)
over five nights, beginning on 2017 November 21.
Six fibre configurations with a similar nominal centre of
RA=92.20°, Dec.=+24.28° were observed. The 'blue' Hydra fibres
were used giving a resolving power of ∼14000. Spectra were recorded
over a ∼400Å interval, centred at ∼6640Å. The FWHM of a
resolution element was sampled by ∼2.3 (binned) CCD pixels of size
0.2Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 124 342 Targets in M35, giving the information from
which the targets were selected, measurements
from the spectra and kinematic membership
probability
table3.dat 165 242 The properties of cluster members (with
pmem>0.95) for which rotation periods and
SED fits are available
tableb1.dat 202 242 Photometry and SED-fitting results for members
of M35 with rotation periods
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/575/A120 : DANCe study of M35 (NGC 2168) (Bouy+, 2015)
J/ApJ/695/679 : Stellar rotation in M35 (Meibom+, 2009)
J/AJ/156/37 : Photometry & Li abund. of cool dwarfs in M35
(Anthony-Twarog+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Source name (JHHMMSSss+DDMMSSs) (G1)
19- 27 F9.6 deg RAdeg Right ascension (J2000)
29- 37 F9.6 deg DEdeg Declination (J2000)
39- 44 F6.3 mag Vmag V-band magnitude
46- 55 F10.7 mag Ksmag Ks-band magnitude
57- 61 F5.3 mag B-V B-V colour
63- 69 F7.3 d Period ? Rotation period
71 I1 --- r_Period ? Source of the rotation period (1)
73- 77 F5.1 --- S/N Signal to noise ratio
79- 84 F6.2 km/s RV Radial velocity
86- 89 F4.2 km/s e_RV Error on RV
91- 95 F5.1 m/s FWHM Full-Width at Half-Maximum
97- 101 F5.1 10-4nm EW(Li) Equivalent width of the Li I 6707.8Å line
103- 106 F4.1 10-4nm e_EW(Li) Error on EW (Li)
108- 112 F5.1 10-4nm EW(Ca) Equivalent width of the Ca I 6717.7Å line
114- 117 F4.1 10-4nm e_EW(Ca) Error on EW (Ca)
119- 124 F6.3 --- pmem Kinematic membership probability (2)
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Note (1): Reference as follows:
1 = Meibom et al. (2009ApJ...695..679M 2009ApJ...695..679M, Cat. J/ApJ/695/679)
2 = Libralato et al. (2016MNRAS.456.1137L 2016MNRAS.456.1137L)
Note (2): -1 indicates missing information or |RV|>50km/s
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Source name (JHHMMSSss+DDMMSSs) (G1)
19- 24 F6.1 K Teff Effective temperature from SED fit
26- 39 F14.11 [Lsun] logL Logarithm of the luminosity from SED fit
41- 54 F14.10 [Lsun] e_logL ?=999 Error on logL
56- 74 F19.17 --- A(Li) NLTE lithium abundance
76- 87 F12.10 --- e_A(Li) Lower error on A(Li) (1)
89- 100 F12.10 --- E_A(Li) Upper error on A(Li) (1)
102- 119 F18.16 --- rho Relative over-radius (2)
121- 128 F8.3 10-4nm DEWLi Deviation of EW(Li) from the trend defined by
slowly rotating stars
130- 139 F10.7 10-4nm e_DEWLi Error on DEWLi
141- 151 F11.8 d Period Rotation period
153- 163 F11.8 [-] logNR Logarithm of the Rossby number (3)
165 A1 --- Binary [0/1] Flag indicating binary status
(1=likely binary)
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Note (1): Error bars of zero indicate an upper limit
Note (2): The over-radius ρ is defined as ρ=sqrt(10ΔlogL) that
corresponds to the factor by which the stellar radius needs to
increase to produce the observed ΔlogL/L☉, assuming no
contribution from a binary companion
Note (3): NR is the ratio of rotation period to convective turnover time
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Source name (JHHMMSSss+DDMMSSs) (G1)
19- 24 F6.3 mag Umag ?=99.999 U-band magnitude (1)
26- 30 F5.3 mag e_Umag ?=9.999 Error on Umag
32- 37 F6.3 mag Bmag ?=99.999 B-band magnitude (1)
39- 43 F5.3 mag e_Bmag ?=9.999 Error on Bmag
45- 50 F6.3 mag Vmag ?=99.999 V-band magnitude (1)
52- 56 F5.3 mag e_Vmag ?=9.999 Error on Vmag
58- 63 F6.3 mag Rcmag ?=99.999 Rc-band magnitude (1)
65- 69 F5.3 mag e_Rcmag ?=9.999 Error on Rmag
71- 76 F6.3 mag Icmag ?=99.999 Ic-band magnitude (1)
78- 82 F5.3 mag e_Icmag ?=9.999 Error on Imag
84- 90 F7.4 mag Gmag Gaia DR2 G-band magnitude
92- 97 F6.4 mag e_Gmag Error on Gmag
99- 105 F7.4 mag BPmag Gaia DR2 BP-band magnitude
107- 112 F6.4 mag e_BPmag Error on BPmag
114- 120 F7.4 mag RPmag Gaia DR2 RP-band magnitude
122- 127 F6.4 mag e_RPmag Error on RPmag
129- 134 F6.3 mag Jmag 2MASS J-band magnitude
136- 140 F5.3 mag e_Jmag Error on Jmag
142- 147 F6.3 mag Hmag 2MASS H-band magnitude
149- 155 F7.3 mag e_Hmag ?=999 Error on Hmag
157- 162 F6.3 mag Ksmag 2MASS Ks-band magnitude
164- 170 F7.3 mag e_Ksmag ?=999 Error on Ksmag
172- 178 F7.3 mag W1mag ?=999 AllWISE W1-band (3.4um) magnitude
180- 186 F7.3 mag e_W1mag ?=999 Error on W1mag
188- 194 F7.3 mag W2mag ?=999 AllWISE W2-band (4.6um) magnitude
196- 202 F7.3 mag e_W2mag ?=999 Error on W2mag
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Note (1): U, B, V, RC, and IC magnitudes were taken where possible from a
recent homogeneous photometric survey of M35
(see Anthony-Twarog et al. 2018AJ....156...37A 2018AJ....156...37A, Cat. J/AJ/156/37)
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Global Notes:
Note (G1): Target names are from Bouy et al. (2015A&A...575A.120B 2015A&A...575A.120B,
Cat. J/A+A/575/A120)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 29-Sep-2023