J/AJ/150/88 Abundances in the local region. I. G and K giants (Luck, 2015)
Abundances in the local region. I. G and K giants.
Luck R.E.
<Astron. J., 150, 88 (2015)>
=2015AJ....150...88L 2015AJ....150...88L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, giant ; Stars, G-type ; Stars, K-type ;
Abundances ; Reddening ; Effective temperatures ; Stars, masses ;
Stars, ages ; Cross identifications
Keywords: Galaxy: abundances - stars: abundances - stars: evolution -
stars: fundamental parameters
Abstract:
Parameters and abundances for 1133 stars of spectral types F, G, and K
of luminosity class III have been derived. In terms of stellar
parameters, the primary point of interest is the disagreement between
gravities derived with masses determined from isochrones, and
gravities determined from an ionization balance. This is not a new
result per se, but the size of this sample emphasizes the severity of
the problem. A variety of arguments led to the selection of the
ionization-balance gravity as the working value. The derived
abundances indicate that the giants in the solar region have Sun-like
total abundances and abundance ratios. Stellar evolution indicators
have also been investigated with the Li abundances and the [C/Fe] and
C/O ratios, indicating that standard processing has been operating in
these stars. The more salient result for stellar evolution is that the
[C/Fe] data across the red-giant clump indicates the presence of
mass-dependent mixing in accord with standard stellar evolution
predictions.
Description:
At the start of this program, the observation list for giants was set
to sample the G/K giants of the local region out to about 100pc from
the Sun in all directions. The region was subdivided into cubes that
were 25pc on a side; from each sub-volume, appropriate stars were
selected north of declination -30°. This sample yielded the 286
G/K giants found in Luck et al. 2007 (cat. J/AJ/133/2464). This data
set was also augmented by the addition of numerous G/K giants,
increasing the number in the 100pc volume to 594 stars. Because the
volume selection criteria used in Luck et al. 2007 (cat.
J/AJ/133/2464) formally extended out to 115pc, a more precise
comparison is that the current sample has 740 stars out to the older
limit. Additional stars from the Bright Star Catalog (Hoffleit &
Jaschek, 1991bsc..book.....H 1991bsc..book.....H) were added, driving the sample out to
about 200pc. The spectral database was supplemented using the ELODIE
and ESO Archives. The ESO addition adds the southern sky. The bulk of
the northern stars were observed using the McDonald Observatory Struve
Telescope and Sandiford Cassegrain Echelle Spectrograph. For the
ELODIE and ESO data archives, a list of all stars available was
obtained and spectral type for each from SIMBAD was retrieved. Stars
having a spectral type of F, G, or K III were then processed. The ESO
data derives from the HARPS and UVES spectrographs. Basic
observational data for the program stars can be found in Table1, along
with some derived quantities, such as distance.
The primary source of observational data for this study is a set of
high signal-to-noise ratio (S/N) spectra obtained during numerous
observing runs between 1997 and 2010 at McDonald Observatory using the
2.1m Struve Telescope and the Sandiford Cassegrain Echelle
Spectrograph. The spectra continuously cover a wavelength range from
about 484 to 700nm, with a resolving power of about 60000. Typical S/N
values for the spectra are in excess of 150. To enable cancellation of
telluric lines, broad-lined B stars were regularly observed with S/N
exceeding that of the program stars. The 726 stars observed with the
Sandiford spectrograph are marked with an "S" in column "Sce" of
Table1.
A further 120 spectra were obtained from the ELODIE Archive. These
echelle spectra are fully processed through order co-addition with a
continuous wavelength span from about 400 to 680 nm and a resolution
of 42000. Only spectra with S/N>50 were utilized in this analysis. An
"E" in Table1, column "Sce", marks these stars.
The ESO Archive was used to obtain spectra from the ESO 3.6m telescope
and HARPS spectrograph. The HARPS spectra cover a continuous
wavelength range from about 400 to 680nm with a native resolving power
of 120000. To match the resolution of the Sandiford data and to
increase the S/N of the data, these spectra were co-added to a
resolution of 60000. Typical maximum S/N values (per pixel) for the
spectra are in excess of 150. In Table1, column "Sce", these stars are
marked with an "H."
Spectra from the UVES spectrograph and VLT/UT2 were also utilized.
These spectra are rather heterogeneous, having resolutions of
40000-80000 and non-continuous spectral coverages in the range
400-700nm. A number of the spectra from UVES stop at about 625nm,
meaning that [O I] 630nm and Li I 670nm were not observed. In Table 1,
"U" denotes the stars observed with UVES spectrograph.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 171 1133 Program stars
table2.dat 91 1146 Reddening, temperature, mass, and age for the
program stars
table3.dat 168 1152 Stellar parameters, Fe, C, O, Li abundance data
table4.dat 186 2296 Average element abundances [x/H]
table5.dat 97 26 Gradients with respect to [Fe/H] for ionization
balance abundances
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2010-)
I/274 : Catalog of Components of Double & Multiple stars (Dommanget+ 2002)
I/259 : The Tycho-2 Catalogue (Hog+ 2000)
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
J/AJ/148/54 : The Hypatia Catalog ((Hinkel+, 2014)
J/PASJ/63/1035 : Stellar parameters and abundances of 99 giants (Wang+, 2011)
J/AJ/142/136 : Spectroscopy of Cepheids. l=30-250° (Luck+, 2011)
J/A+A/526/A71 : C abundances in G and K nearby stars (da Silva+, 2011)
J/A+A/503/541 : Neutral Li in late-type stars NLTE calculations (Lind+, 2009)
J/A+A/475/1003 : Stellar parameters of G and K giant stars (Hekker+, 2007)
J/AJ/133/2464 : Parameters and abundances of nearby giants (Luck+, 2007)
J/AJ/129/1063 : Abundances of stars within 15pc of the Sun (Luck+, 2005)
J/MNRAS/349/757 : Masses, ages and metallicities of F-G dwarfs (Lambert+, 2004)
http://bifrost.astr.cwru.edu/FGKasp/index2.php : The FGK Stars Spectral Library
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Identifier from SIMBAD database
25- 31 A7 --- HD HD number
33- 38 I6 --- HIP [343/118209]? HIP number (cat. I/239)
40- 43 I4 --- HR [2/9104]? HR number
45- 55 A11 --- CCDM Identifier in the Catalog of Components of
Double & Multiple stars identifier (cat. I/274)
56- 58 A3 --- m_CCDM CCDM component (A, AB, ABC, AC, AP, B, or D)
60- 78 A19 --- OName Other name (cluster designation from SIMBAD)
80- 82 A3 --- Sce Source of spectroscopic material (S=Sandiford,
E=ELODIE, H=HARPS, U=UVES) (G1)
84-106 A23 --- Key Key name(s) (1)
108-121 A14 --- SpT Simbad spectral type
123-136 A14 --- Type Simbad object type
138-143 F6.3 mag Vmag [-0.05/12.2]? Simbad V-band magnitude
145-149 F5.3 mag B-V [0/2.1]? Simbad (B-V) color index
151-156 F6.2 arcsec plx [-0.4/111]? Simbad parallax
158-163 F6.1 pc Dist [9/3125]? Simbad distance
165-171 F7.2 km/s RV [-184.4/183.4]? Simbad radial velocity
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Note (1): Identifier used in subsequent tables to identify stars. The tag in
some cases provides an alternate identification for the object. If a star
has multiple sources, there will be a matching keyname for each.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Simbad identifier
25 A1 --- Sce [ESHU] Spectroscopic material source
(S=Sandiford, E=ELODIE, H=HARPS, U=UVES) (G1)
27- 31 F5.3 mag E(B-V) [0/0.5]? The (B-V) color excess (1)
33- 36 I4 K Teff [3764/7728]? Adopted effective temperature (2)
38- 41 I4 K e_Teff [0/1011]? The standard deviation in Teff
43- 44 I2 --- o_Teff [0/16] Number of colors used to determine Teff
46- 50 F5.2 [Lsun] logL [-0.5/4.1]? Log luminosity (Log(L/L☉) (3)
52- 55 F4.2 Msun BMass [0.8/4.2]? Mass derived from Bertelli et al.
1994 (cat. J/A+AS/106/275) isochrone
57- 60 F4.2 Msun DMass [0.6/3.3]? Mass derived from Dotter et al.
(2008ApJS..178...89D 2008ApJS..178...89D) isochrone
62- 65 F4.2 Msun YMass [0.7/3.9]? Mass derived from Demarque et al.
(2004ApJS..155..667D 2004ApJS..155..667D) isochrone
67- 70 F4.2 Msun <Mass> [0.7/3.6]? Mean mass from all determinations
72- 76 F5.2 Gyr BAge [0.1/11.7]? Age derived from Bertelli et al.
1994 (cat. J/A+AS/106/275) isochrone
78- 81 F4.2 Gyr DAge [0.3/9.4]? Age derived from Dotter et al.
(2008ApJS..178...89D 2008ApJS..178...89D) isochrone
83- 86 F4.2 Gyr YAge [0.2/9]? Age derived from Demarque et al.
(2004ApJS..155..667D 2004ApJS..155..667D) isochrone
88- 91 F4.2 Gyr <Age> [0.2/9.4]? Mean age from all determinations
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Note (1): Computed using the reddening maps of Hakkila et al.
(1997AJ....114.2043H 1997AJ....114.2043H), the parallax distance, and a correction for the lack
of reddening within 75pc.
Note (2): Derived using the calibration of Ramirez & Melendez
(2005ApJ...626..465R 2005ApJ...626..465R).
Note (3): Derived from the distance, apparent V magnitude, and the bolometric
corrections of Bessell, Castelli, & Plez (1998A&A...333..231B 1998A&A...333..231B).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Key Key name (see Table1 for cross identification)
17 A1 --- Sce [ESHU] Source of spectra (S=Sandiford, E=ELODIE,
H=HARPS, U=UVES) (G1)
19- 22 I4 K Teff1 [3764/7728]? Group 1 effective temperature (1)
24- 27 F4.2 [cm/s2] logg1 [0.06/4.9]? Log group 1 surface gravity
29- 32 F4.2 km/s Vt1 [0/6.5]? Group 1 microturbulent velocity
34- 38 F5.2 [Sun] FeI1 [-2.3/1.2]? Group 1 [Fe/H] from Fe I lines (2)
40- 43 F4.2 [Sun] e_FeI1 [0.05/0.7]? Standard deviation in FeI1
45- 47 I3 --- o_FeI1 [7/676]? Number of Fe I lines used in FeI1
49- 53 F5.2 [Sun] FeII1 [-2.2/1.7]? Group 1 [Fe/H] from Fe II lines (2)
55- 58 F4.2 [Sun] e_FeII1 [0/1.3]? Standard deviation in FeII1
60- 61 I2 --- o_FeII1 [1/95]? Number of Fe II lines used in FeII1
63- 66 F4.2 [-] C1 [6.4/10]? Group 1 carbon abundance (3)
68- 72 F5.2 [-] O1 [7.8/10.3]? Group 1 oxygen abundance (3)
74- 78 F5.2 [-] Li1 [-1.6/3.6]? Groupt 1 lithium abundance (3)
80- 84 F5.2 pm EW1 [0.04/50.8]? Group 1 Li I 6707Å equivalent
width (4)
86- 90 F5.2 --- Li1c [-0.15/3.3]? Group 1 non-LTE lithium abundance
correction (5)
92- 95 I4 K Teff2 [3764/7728]? Group 2 effective temperature (6)
97-101 F5.2 [cm/s2] logg2 [-1/5]? Log group 2 surface gravity
103-106 F4.2 km/s Vt2 [0.2/7.75]? Group 2 microturbulent velocity
108-112 F5.2 [Sun] FeI2 [-2.3/1.2]? Group 2 [Fe/H] from Fe I lines (2)
114-117 F4.2 [Sun] e_FeI2 [0.04/0.7]? Standard deviation in FeI1
119-121 I3 --- o_FeI2 [7/676]? Number of Fe I lines used in FeI1
123-127 F5.2 [Sun] FeII2 [-2.3/1.2]? Group 2 [Fe/H] from Fe II lines (2)
129-132 F4.2 [Sun] e_FeII2 [0.02/1.4]? Standard deviation in FeII1
134-135 I2 --- o_FeII2 [1/95]? Number of Fe II lines used in FeII1
137-140 F4.2 [-] C2 [6.6/8.8]? Group 2 carbon abundance (3)
142-146 F5.2 [-] O2 [7.4/10.1]? Group 2 oxygen abundance (3)
148-152 F5.2 [-] Li2 [-1.7/3.6]? Group 2 lithium abundance (3)
154-158 F5.2 --- Li2c [-0.9/1.6]? Group 2 non-LTE lithium abundance
correction (5)
160-164 F5.1 km/s Vbroad [1.7/150] Broadening velocity
166 A1 --- Broad [GR] Type of broadening (G=Gaussian
macroturbulence, R=Rotational)
168 I1 --- Clump [1/2] Clump star flag (1=True, 2=False)
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Note (1): All group 1 for the mass determined gravity.
Note (2): With respect to the solar value =7.47.
Note (3): With respect to log(εH)=12.
Note (4): EW1<1.00pm corresponds to an upper limit.
Note (5): From the data of Lind et al. 2009 (cat. J/A+A/503/541).
Note (6): All group 2 is the ionization balance determined gravity.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Type Data type (M=Mass determined gravity data,
IB=Ionization balance determined gravity data)
4- 18 A15 --- Key Key name (see Table1 for cross identification)
20 A1 --- Sce Source of spectra (S=Sandiford, E=ELODIE,
H=HARPS, U=UVES) (G1)
22- 25 I4 K Teff Effective temperature
27- 31 F5.2 [cm/s2] logg Log surface gravity
33- 36 F4.2 km/s Vt Microturbulent velocity
38- 42 F5.2 [Sun] Na ? Log sodium abundance
44- 48 F5.2 [Sun] Mg ? Log magnesium abundance
50- 54 F5.2 [Sun] Al ? Log aluminum abundance
56- 60 F5.2 [Sun] Si Log silicon abundance
62- 66 F5.2 [Sun] S ? Log sulfur abundance
68- 72 F5.2 [Sun] Ca ? Log calcium abundance
74- 78 F5.2 [Sun] Sc ? Log scandium abundance
80- 84 F5.2 [Sun] Ti Log titanium abundance
86- 90 F5.2 [Sun] V ? Log vanadium abundance
92- 96 F5.2 [Sun] Cr ? Log chromium abundance
98-102 F5.2 [Sun] Mn ? Log manganese abundance
104-108 F5.2 [Sun] Fe Log iron abundance
110-114 F5.2 [Sun] Co ? Log cobalt abundance
116-120 F5.2 [Sun] Ni Log nickel abundance
122-126 F5.2 [Sun] Cu ? Log copper abundance
128-132 F5.2 [Sun] Zn ? Log zinc abundance
134-138 F5.2 [Sun] Sr ? Log strontium abundance
140-144 F5.2 [Sun] Y ? Log yttrium abundance
146-150 F5.2 [Sun] Zr ? Log zirconium abundance
152-156 F5.2 [Sun] Ba ? Log barium abundance
158-162 F5.2 [Sun] La ? Log lanthanum abundance
164-168 F5.2 [Sun] Ce ? Log cerium abundance
170-174 F5.2 [Sun] Nd ? Log neodymium abundance
176-180 F5.2 [Sun] Sm ? Log samarium abundance
182-186 F5.2 [Sun] Eu ? Log europium abundance
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- El Element identifier
5- 9 F5.3 --- Slope1 Gradient group 1 slope (1)
11- 16 F6.3 --- Int1 Gradient group 1 intercept (1)
18- 22 F5.3 --- e_Slope1 Standard error of Slope1
24- 28 F5.3 --- e_Int1 Standard error of Int1
30- 34 F5.3 --- Sigma1 Standard deviation of gradient group 1 fit
(Σ)
36- 41 F6.3 --- Mean1 Mean of gradient group 1 ratios
43- 47 F5.3 --- sigma1 Standard deviation of gradient group 1 mean
49- 54 F6.3 --- Slope2 ? Gradient group 2 slope (2)
56- 61 F6.3 --- Int2 ? Gradient group 2 intercept (2)
63- 67 F5.3 --- e_Slope2 ? Standard error of Slope2
69- 73 F5.3 --- e_Int2 ? Standard error of Int2
75- 79 F5.3 --- Sigma2 ? Standard deviation of gradient group 2 fit
(Σ)
81- 86 F6.3 --- Mean2 ? Mean of gradient group 2 ratios (3)
88- 92 F5.3 --- sigma2 ? Standard deviation of gradient group 2 mean
94- 97 I4 --- Nstar Number of stars
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Note (1): Gradient of the form: [Element/H] = Slope1*[Fe/H]+Int1.
The slopes all tend to be near 1 and the intercept (Int1) is about mean
value (Mean1) in the local region.
Note (2): Gradient of the form: [Element/Fe] = Slope2*[Fe/H]+Int2. The slope
should be about 0, with the intercept having the local region [Element/Fe]
value.
Note (3): The mean of the [Element/Fe] values and is close to Int2 in value.
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Global notes:
Note (G1): The codes for the spectroscopic material are defined as below:
S = McDonald Observatory Struve Reflector and Sandiford echelle spectrograph;
E = Observatoire d'Haute Provence ELODIE spectrograph;
H = European Southern Observatory HARPS spectrograph;
U = European Southern Observatory UVES spectrograph.
History:
From electronic version of the journal
References:
Luck et al., Paper II 2017AJ....153...21L 2017AJ....153...21L, Cat. J/AJ/153/21
Luck et al., Paper III 2018AJ....155..111L 2018AJ....155..111L
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 16-Oct-2015