J/AJ/153/128 WOCS. LXXV. Hyades&Praesepe stellar lithium data (Cummings+, 2017)
WIYN open cluster study.
LXXV. Testing the metallicity dependence of stellar lithium depletion using
Hyades-aged clusters.
I. Hyades and Praesepe.
Cummings J.D., Deliyannis C.P., Maderak R.M., Steinhauer A.
<Astron. J., 153, 128-128 (2017)>
=2017AJ....153..128C 2017AJ....153..128C (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Stars, double and multiple ;
Photometry, UBV ; Abundances ; Effective temperatures ;
Equivalent widths ; Radial velocities
Keywords: open clusters and associations: individual: The Hyades, Praesepe -
stars: abundances - stars: evolution
Abstract:
WIYN/Hydra spectroscopy (at R∼15000) of the moderately metal-rich Praesepe
and Hyades open clusters was used to study their main-sequence (MS)
iron ([Fe/H]) and lithium (A(Li)) abundances. Self-consistent [Fe/H]
and Li analyses of these clusters of consistent age, which we re-evaluate,
confirms that they have consistent [Fe/H] and provides a foundation to
investigate the poorly understood G-dwarf and F-dwarf Li-depletions.
Neither phenomenon agrees with standard stellar evolution theory, but
possible explanations abound. We supplement our A(Li) with previously
published results placed on a uniform abundance scale. This creates
the largest self-consistently analyzed sample of A(Li) in both the
Hyades (90) and Praesepe (110). For each star, high-precision UBVRI
photometry was used to determine a 10-color-based Teff and then to
test for photometric peculiarities indicated by a large σTeff
(>75 K). The stars that have large σTeff were predominantly
found to be binaries or stars with peculiar (apparent) A(Li). When
considering only proper-motion members that have low σTeff and
are also photometrically consistent with the cluster MS fiducial, each
cluster has a more tightly defined Li morphology than previously
observed and the two clusters' A(Li) are indistinguishable. This
suggests that clusters of consistent age and metallicity may have
consistent Li-depletion trends across a broad range of Teff; no
additional major parameters are required, at least for these two
clusters. We propose that the combined Hyades and Praesepe data offer
more rigorous constraints than does either cluster alone, and we
discuss newly revealed features of the combined Li-Teff trend.
Description:
The Hyades and Praesepe open star clusters were both observed using
the Hydra multi-object spectrograph on the WIYN 3.5-meter telescope
using the 316@63.4 echelle grating in order 8 with the X19 filter. The
spectra span from 6450 to 6850 Å. All Hyades stars and a majority of
Praesepe stars were observed with blue cable, which yielded R∼13600.
The remaining Praesepe stars were observed with the red cable, which
yielded a moderately higher R∼17600.
The Hyades data were acquired over seven nights from 2009 February 2 to 23.
Using two red-cable configurations, we obtained spectra of 34 Praesepe
candidate cluster members on 1997 November 16 and 18. Using seven blue
cable configurations, we obtained spectra of 66 candidate cluster members
during seven nights on 2001 December 2; 2005 May 1 and 2; 2006 January 25
and 26; and 2006 February 2 and 3.
Objects:
------------------------------------------------------------
RA (ICRS) DE Designation(s)
------------------------------------------------------------
04 26 54.00 +15 52 00.0 Hyades = NAME Hyades Cluster
08 40 24 +19 40.0 Praesepe = NGC 2632
------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table6.dat 105 90 Stellar Lithium Data for The Hyades
table7.dat 105 110 Stellar Lithium Data for Praesepe
--------------------------------------------------------------------------------
See also:
J/AJ/106/1080 : Lithium in Praesepe (Soderblom+, 1993)
J/A+A/310/879 : Hyades binaries (Barrado+, 1996)
J/A+A/331/81 : Hyades membership (Perryman+ 1998)
J/ApJ/521/682 : Binaries in the Praesepe and Coma clusters (Abt+, 1999)
J/A+A/354/881 : Radial velocities of Praesepe + Hyades Am stars
(Debernardi+ 2000)
J/AJ/122/1486 : NGC 2451A proper motions and membership (Platais+, 2001)
J/A+A/382/899 : BVI photometry in M67 (Stassun+, 2002)
J/AJ/124/601 : Absolute positions and proper motions in NGC 188
(Platais+, 2002)
J/AJ/126/2922 : Astrometry and membership in NGC 188 (Platais+, 2003)
J/AJ/127/3579 : Radial velocities of Hyades stars (Paulson+, 2004)
J/ApJS/159/100 : Temperatures and Rc photometry in the Hyades (Taylor+, 2005)
J/A+A/461/509 : Membership and spectroscopy of IC 2391 (Platais+, 2007)
J/A+A/484/609 : BVI photometry and proper motions in M67 (Yadav+, 2008)
J/AJ/135/2264 : Stellar radial velocities in NGC 188 (Geller+, 2008)
J/MNRAS/391/1482 : BVIc photometry of Trumpler 20 (Platais+, 2008)
J/A+A/498/949 : Velocities of 1253 F-K dwarfs in open clusters
(Mermilliod+, 2009)
J/AJ/137/3743 : Spectroscopic binary orbits in NGC 188 (Geller+, 2009)
J/AJ/137/5086 : NGC 188 V12 VI light curves (Meibom+, 2009)
J/AJ/138/159 : NGC 6819 stellar radial-velocity and photometry
(Hole+, 2009)
J/ApJ/695/679 : Stellar rotation in M35 (Meibom+, 2009)
J/A+A/515/A100 : VI light curves of NGC 1039 solar-type stars (James+, 2010)
J/AJ/139/1383 : Radial velocities in M35 (NGC 2168) (Geller+, 2010)
J/AJ/139/2034 : NGC 6253 stars equivalent widths (Anthony-Twarog+, 2010)
J/A+A/531/A92 : Deep all-sky census of the Hyades (Roeser+, 2011)
J/ApJ/733/115 : Rotation periods and membership in M34 (Meibom+, 2011)
J/MNRAS/413/1024 : Deep proper-motion survey of Blanco 1 (Platais+, 2011)
J/MNRAS/413/2218 : Stellar rotation in Hyades and Praesepe (Delorme+, 2011)
J/A+A/541/A150 : Lithium in M67 and Hyades (Pace+, 2012)
J/AJ/146/43 : WIYN open cluster study. LV. NGC 6819 (Platais+, 2013)
J/AJ/148/38 : WIYN open cluster study. LX. RV survey of NGC 6819
(Milliman+, 2014)
J/AJ/148/51 : WIYN Open Cluster. LXI. NGC 6819 photometry
(Anthony-Twarog+, 2014)
J/AJ/148/61 : WIYN open cluster study. LIX. RVs of NGC 6791
(Tofflemire+, 2014)
J/AJ/148/85 : WIYN open cluster study. LXII. Photometry of M35
(Thompson+, 2014)
J/ApJ/784/57 : Photometry and proper motions in Praesepe (Wang+, 2014)
J/ApJ/795/161 : Activity and rotation in Praesepe and the Hyades
(Douglas+, 2014)
J/AJ/149/121 : WOCS. LXV. Abundances in NGC 6819 (Lee-Brown+, 2015)
J/AJ/150/10 : WOCS. LXVI. Radial velocity survey in M35 (Leiner+, 2015)
J/AJ/150/97 : Radial velocities in M67. I. 1278 candidate members
(Geller+, 2015)
J/AJ/151/152 : WOCS. LXXI. Spectroscopy of 5 stars in NGC 6791
(Milliman+, 2016)
J/AJ/152/192 : WOCS. LXXII. A uvbyCaHb study of NGC 2506
(Anthony-Twarog+, 2016)
Byte-by-byte Description of file: table6.dat table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Group [ABCD] Data group (1)
3- 11 A9 --- ID Star identifier (vB NNN, for most stars
in table 6; KW NNN in table 7)
13 A1 --- n_ID [ab] Note on ID (2)
15- 19 F5.3 mag (B-V)mean [0.194/1.225] Mean (B-V) color index
21- 26 F6.1 K Teff [4301.9/7623] Effective temperature
28- 32 F5.1 K e_Teff [6.3/373.9]? Uncertainty in Teff
33 A1 --- n_Teff [*] Note on Teff (only in table 6) (3)
35- 40 F6.2 0.1pm EW(Li) [3/121.06]? Lithium equivalent width (mÅ)
42- 45 F4.2 0.1pm e_EW(Li) [0.59/5.93]? Uncertainty in EW(Li)
47- 51 F5.3 [-] A(Li) [0/3.41] Lithum abundance
53- 57 F5.3 [-] e_A(Li)S/N [0.005/0.097]? S/N-based uncertainty for
A(Li)
59- 63 F5.3 [-] e_A(Li)Teff [0.01/0.269]? Teff-based uncertainty for
A(Li)
65- 68 I4 --- S/N [120/1500]? Signal-to-noise ratio per pixel
70- 74 I5 s Exp1 [150/10945]? Total exposure time (only
in table 6)
76- 80 A5 "h:m:s" Exp2 ? Total exposure time (only in table 7)
82 A1 --- l_vsini [<] Limit flag on vsini
83- 87 F5.1 km/s vsini [1.5/210]? Rotational broadening (4)
89- 93 F5.2 km/s RV [17.8/64.53]? Radial velocity (5)
95- 99 F5.2 km/s e_RV [0.06/24.43]? 1σ uncertainty in RV
101 I1 --- Ref [1/9] Reference (6)
103-105 A3 --- Prime [yes-] Prime sample member? (7)
--------------------------------------------------------------------------------
Note (1): Group as follows:
A = Single-star detection;
B = Spectroscopic binary based on Perryman et al. (1998, J/A+A/331/81; and
references therein);
C = Single-star 3σ upper limit;
D = Spectroscopic binary 3σ upper limit.
Note (2): Note as follows:
a = Short Period Tidally Locked Binary (SPTLB);
b = Star that deviate from the single-star fiducial (see Figure 3).
Note (3): Note as follows:
* = 13 of the stars we analyzed from Thorburn et al. (1993ApJ...415..150T 1993ApJ...415..150T),
Boesgaard & Tripicco (1986ApJ...302L..49B 1986ApJ...302L..49B) and Boesgaard & Budge
(1988ApJ...332..410B 1988ApJ...332..410B) have clearly discrepant photometry in comparison to
the Hyades MS fiducial in MV space. Therefore, their Teff was not
determined using our derived color relations because they would not be
appropriate. Their final Teff are thus based only on their
Johnson & Knuckles (1955ApJ...122..209J 1955ApJ...122..209J) B-V and they have increased
uncertainty.
Note (4): In table 6, the source for vsini of the Boesgaard & Tripicco
(1986ApJ...302L..49B 1986ApJ...302L..49B) and Boesgaard & Budge (1988ApJ...332..410B 1988ApJ...332..410B) stars (3)
are Kraft (1965ApJ...142..681K 1965ApJ...142..681K) but scaled to our measurements. The source
for vsini of the Burkhart & Coupry (1989A&A...220..197B 1989A&A...220..197B) stars (5) are
Debernardi et al. (2000, J/A+A/354/881).
In table 7, the source for v sin i of stars we did not observe is
Mermilliod et al. (2009, J/A+A/498/949).
Note (5): In table 6, the source for radial velocities of stars we did not
observe is Perryman et al. (1998, J/A+A/331/81) (and references therein) and
for vB 99 and vB 182 it is Griffin et al. (1988AJ.....96..172G 1988AJ.....96..172G).
In table 7, the source for radial velocities of stars we did not
observe is Mermilliod et al. (2009, J/A+A/498/949).
Note (6): Reference as follows:
1 = Our WIYN/Hydra sample;
2 = Thorburn et al. (1993ApJ...415..150T 1993ApJ...415..150T);
3 = Boesgaard & Budge (1988ApJ...332..410B 1988ApJ...332..410B) and Boesgaard & Tripicco
(1986ApJ...302L..49B 1986ApJ...302L..49B);
4 = Soderblom et al. (1990AJ.....99..595S 1990AJ.....99..595S);
5 = Burkhart & Coupry (1989A&A...220..197B 1989A&A...220..197B);
6 = Takeda et al. (2013PASJ...65...65T 2013PASJ...65...65T);
7 = Boesgaard et al. (2013ApJ...775...58B 2013ApJ...775...58B);
8 = Soderblom et al. (1993, J/AJ/106/1080);
9 = Burkhart & Coupry (1998A&A...338.1073B 1998A&A...338.1073B).
Note (7): For each cluster, we define a "prime" subsample consisting of probable
members with low e_Teff and no measurable spectroscopic evidence of
contamination from a secondary (from fxcor), even if they are known binaries
from other studies.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
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(End) Tiphaine Pouvreau [CDS] 14-May-2018