Giants in the Local Region

R. Earle Luck and Ulrike Heiter

Reference: Astronomical Journal, 133, 2464, 2007 June

The published version of the paper contains only the stubs to Tables 1-4, 6, and 7. Machine readable versions are available for these tables online from the Astronomical Journal site but human readable versions are not available online. We present here human readable as well as alternately formatted versions of all tables from the paper.

 

Table 1.  Program Stars

 

HIC              Hipparchos Number

HD               Henry Draper Number

HR               Bright Star Number

mV                Apparent Magnitude

MV               Absolute magnitude computed using the parallax derived distance

SpTy            Spectral type (primary source Hipparchos (ESA 1997))

Parallax      From Hipparchos

Distance     From parallax

L                  Galactic longitude

B                  Galactic latitude

RV               Radial Velocity and its error

RV_e           Radial Velocity uncertainty

S                   Source for radial velocity:  L = this work, F = Famaey et al. (2005), M = de Mederios & Mayor (1999)

SB                Spectroscopic Binary – classification from de Mederios & Mayor (1999)

 

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Table 2.  Parameters and Iron Abundances

 

HIC            Hipparchos Number

HD             Henry Draper Number

HR             Bright Star Number

Teff,             Spectroscopic effective temperature in Kelvins

log g         Spectroscopic logarithmic surface gravity (cm/s2)

Vt,              Spectroscopic microturbulent velocity (km/s)

[Fe/H]       Spectroscopic mean logarithmic iron abundance relative to the Sun

σ                 Standard deviation about the mean [Fe/H] ratio

N                Number of lines (Fe I) in the determination

Teff                  MARCS75 effective temperature in Kelvins

log g         MARCS75 logarithmic surface gravity (cm/s2)

Vt,              MARCS75 microturbulent velocity (km/s)

[Fe/H]      MARCS75 mean logarithmic iron abundance relative to the Sun

Teff                  Physical effective temperature in Kelvins

log g        Physical logarithmic surface gravity (cm/s2)

Vt,              Physical microturbulent velocity (km/s)

[FeI/H]      Physical mean logarithmic iron abundance as determined from Fe I relative to the Sun

[FeII/H]    Physical mean logarithmic iron abundance as determined from Fe II relative to the Sun

 

Both spectroscopic and physical analyses use MARCS models (2002) while the MARCS75 analysis uses the 1975 MARCS model atmospheres.

 

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Table 3:  Mass and Luminosity Estimates

 

HIC          Hipparchos Number

HD           Henry Draper Number

HR           Bright Star Number

MV           Absolute Johnson V magnitude as computed from the Hipparchos parallax

MV_e       Abolute magnitude uncertainty as computed from the Hipparchos parallax error.

Mass        Stellar mass in solar masses.

Mbol         Bolometric absolute magnitude.

LSun         Logarithm of the stellar luminosity in solar units.

log g        Surface gravity in cm/s2.

 

There are three sets of Mass, Mbol, LSun, and log g corresponding to:

 

Physical:  Mass and bolometric magnitude derived using the isochrones of Bertelli et al. (1994) that are interpolated using the absolute V magnitude and photometric temperature.  LSun and log g then derived using standard relations.

 

Spectroscopic Inversion:  The spectroscopic temperature is used to determine the bolometric correction using Bessel, Castelli & Plez (1998).  Mass is then determined using the spectroscopic value for the surface gravity (log g) and the luminosity using the standard relations.

 

Spectroscopic:  Mass and bolometric magnitude derived using the isochrones of Bertelli et al. (1994) that are interpolated using the absolute V magnitude and spectroscopic temperature.  LSun and log g then derived using standard relations.

 

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Table 4.  Average Abundances with Respect to H

 

Column 1:            Star ID

 

Part 1:    Mean Abundances for Na, Mg, Al, Si, S, Ca

Part 2:    Mean Abundances for  Sc, Ti, V, Cr, Mn, Fe

Part 3:    Mean Abundances for Co, Ni, Cu, Zn, Sr, Y

Part 4:    Mean Abundances for Ba, LA, Ce, Pr, Nd, Eu

 

Each element has 3 columns corresponding to:

 

S = Spectroscopic parameters with MARCS models.

M = Spectroscopic parameters with MARCS75 models.

P = Physical parameters with MARCS models

 

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Table 5.  Abundance Uncertainties

 

Mean:        Mean value for the row quantity.  For Species rows this is the mean abundance ([x/H]) for the given species. For σ rows this is the mean of all the individual standard deviations.  For SE rows this is the mean of all the individual standard errors.  For N rows this is the mean number of lines used for the determination of the species abundance.

Median:    Median values in the same sense as the Mean.

σ                 Standard deviation of the Mean.

Max           Maximum value in the same sense as the Mean.

Min            Minimum value in the same sense as the Mean.

N                Number of stars.

 

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Table 6. Lithium Abundance Data

 

HIC        Hipparchos Number

HD         Henry Draper Number

HR         Bright Star Number

TS           Effective temperatures (K) for the spectroscopic analysis parameters

TM             MARCS75 effective temperature

TP           Physical effective temperature

VM          Macroturbulent or rotational velocity (km/s)

T             Broadening type:  G = Gaussian macroturbulence. R = Rotation. 

EW         Li equivalent width in .  Lithium EW is for the synthesized combined components.

S             Spectroscopic parameter Li Abundance.  Abundances are log ε where log ε(H) = 12.

M75       MARCS75 parameter Li Abundance

P             Physical parameter Li abundance

Q            A – D are quality of fit with A the best fit.  L denotes an abundance limit.

 

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Table 7.  CNO Data for Giants

 

HIC               Hipparchos Number

HD                 Henry Draper Number

HR                 Bright Star Number

C                    Carbon abundance (log ε) where H = 12.

N                    Nitrogen abundance (log ε) where H = 12.

O                    Oxygen abundance (log ε) where H = 12.

[C/H]             Carbon abundance relative to the Sun

[N/H]             Nitrogen abundance relative to the Sun

[O/H]             Oxygen abundance relative to the Sun

[C/Fe]            Carbon abundance normalized to the Fe content

[N/Fe]            Nitrogen abundance normalized to the Fe content

[O/Fe]            Oxygen abundance normalized to the Fe content.

CNO              ∑ C + N + O

[CNO/H]       Sum CNO relative to the Sun

[CNO/Fe]     Sum CNO nomalized to the fe content

CN                 ∑ C + N

[CN/H]          Sum CN relative to the Sun

[CN/Fe]         Sum CN nomalized to the fe content

C/O                10**(C-O)

 

There are three sections for this table:  Part 1 has the CNO data derived using spectroscopic parameters, Part 2 uses MARCS75 parameters, and Part 3 Physical parameters.

 

CNO abundances relative to the Sun using solar CNO determined using a solar reflection spectrum and MARCS and MARCS75 models.  For MARCS models solar C, N, O = 8.50, 8.18, 8.81 and for MARCS75 solar C, N, O = 8.42, 8.16, and 8.75 except for Teff > 6200 where C = 8.38 and 8.52 respectively.

 

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Table 8.  Parameter and Iron Abundance Difference and Regression Analysis

 

Mean differences and parameter dependences for this work versus other analyses.

 

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Table 9.  Mean Abundance Data

 

Mean spectroscopic abundances ratios ([x/H] and [x/Fe]) and regression coefficients (a,b) for [x/H] = a*[Fe/H]+b. [x/Fe] = (Slope-1)*[Fe/H] + Intercept where x is the element and Slope and Intercept are taken from the linear regression solution for [x/H] versus [Fe/H].  The uncertainties are identical.

 

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