Auxillary Data

1. Astrophysical gf values for 2224 metal lines

In Gustafsson et al. (2008) almost all metal line opacity data used in the construction of the MARCS model atmospheres was obtained from VALD 1 (Piskunov et al. 1995) and VALD 2 (Stempels et al. 2001). For for 948 atomic lines in VALD 1, and 1276 lines of the 10 most important revised species (Si I, Ca I, Ca II, Ti II, Cr I, Cr II, Mn II, Fe I, Fe II, and Ni II) in VALD 2, however, we obtained and used astrophysical gf values to improve the detailed line spectrum fit to the solar spectrum.

The modified lines fall in the wavelength range 3783 to 8968 Å, and are based on ocular inspection of fits of synthetic solar intensity spectra calculated with the Holweger & Müller (1974) model to the observed solar disk-center FTS spectrum of Brault & Neckel (1987). About 40% of the modified lines are Fe I lines. The most common modifications to the log gf values are negative, since a too strong synthetic line is probably wrong, while a too weak line may be correct and explained by unidentified line blends. A log gf value was only increased when some alternative line identification supported that of the wavelength coincidence. A log gf value of -9.99 signals that the line was not found in the solar spectrum.

This Readme text can be downloaded as astroph_gfVALD.txt.

The plain text data tables astroph_gfVALD1.dat and astroph_gfVALD2.dat give for each line :

1. Element number in the periodic table
2. Ion (1 for neutral, 2 for singly ionized)
3. VALD air wavelength (A) (VALD 1 or VALD 2, respectively)
4. Lower level excitation energy (eV) (VALD 1 or VALD 2, respectively)
5. Lower level j quantum number (VALD 1 or VALD 2, respectively)
6. Astrophysical value of log gf (elaborated to within 0.1 dex)
7. Species label
8. Lower level designation (VALD 1 or VALD 2, respectively)
9. Upper level designation (VALD 1 or VALD 2, respectively)
10. Original VALD log gf (VALD 1 or VALD 2, respectively)

Example: The beginning of file astroph_gfVALD1.dat :

        28 1 3783.5240  0.4230  2.0  -1.70 'Ni I ' 'a 1D       ' 'z 5F*      ' -1.310

        60 2 3784.2450  0.3800  5.5  -0.05 'Nd II' '6s  4I     ' '6p *       '  0.098

        22 1 3789.2940  1.4600  4.0  -0.75 'Ti I ' '(4F)4s b3F ' '(3P)sp u3D ' -0.451

        12 1 3789.5690  4.3460  1.0  -9.99 'Mg I ' 's3p  1P    ' '22d  1D    ' -2.000

        12 1 3793.1630  4.3460  1.0  -9.99 'Mg I ' 's3p  1P    ' '21d  1D    ' -2.000

        22 1 3795.8940  1.4430  3.0  -0.15 'Ti I ' '(4F)4s b3F ' '(3P)sp u3D ' -0.295

        40 2 3796.4930  1.0110  4.5  -0.90 'Zr II' '4d3 a2G    ' 'd25p z2G   ' -0.830

        12 1 3797.1690  4.3460  1.0  -9.99 'Mg I ' 's3p  1P    ' '20d  1D    ' -2.000

        40 2 3800.7430  0.5270  1.5  -2.05 'Zr II' 'd25s a2D   ' 'd25p z4F   ' -1.300

        58 2 3801.5260  0.8970  5.5  -0.05 'Ce II' 'fd6s *4G   ' 'fd6p  4H   '  0.870

        The reference for the astrophysical gf values is Gustafsson et al. (2008).

        The VALD line data base may be found e.g. at http://vald.astro.uu.se/
        

2. Scaled FeH line data

The FeH line list (here generated 15-Jun-2015) was originally calculated by B. Plez for the work on M dwarf stars by Önehag et al. (2012).

• F4Δ - X4Δ transitions
• v'=0,1,2 v"=0,1,2
• Jmax=40.5

where ' and " designate the upper and lower level, respectively. Energy levels were computed from identified levels in Phillips et al. (1987) in the following way: For each vibrational level, and each of the 8 lambda-doubled substates, a fit of energy as a function of rotational quantum numbers (J) was made through the measured rotational levels. In most cases this fit is of order 3, but for a few levels a better quadratic fit was adopted. The calculated levels were only used when no observation was available. Line intensities were computed from Hönl-London and Franck-Condon factors (see Plez (1998) for additional details), and then scaled to agree with the Av'v" of Langhoff & Bauschlicher (1990). The line list is given in the Turbospectrum format. (Turbospectrum can be found at http://ascl.net/1205.004):

        lambda      E"   log(gf)      2*J'+1                            v' v" branch J" species band

          (A)      (eV)

        7626.509  0.086 -4.789  0.00   20.0 0.00E+00 'X' 'X'  0.0  1.0 ' 2  0 SR32  8.5 FeH     FX'
        

Branch designation has its usual meaning, the first and second letter denoting respectively DeltaN and DeltaJ, with Delta=-2,-1,0,1,2 denoted by O,P,Q,R,S. The two numbers are for the four substates. The non-designated columns contain specific but unknown parameters that may be used in Turbospectrum.
The plain text FeH Readme file is FeH_Readme.txt
The plain text data table containing 19830 FeH lines is FeH_Plez_Langhoff-Bauschlicher_strength.dat

References:

• Gustafsson B., Edvardsson B., Eriksson K., Jørgensen U.G., Nordlund Å., Plez B. 2008, A&A 486, 951
• Holweger H., Müller E.A., 1974, Solar Physics 39, 19
• Langhoff S.R., & Bauschlicher C.W. 1990, J. Mol. Spectrosc. 141, 243
• Önehag A., Heiter U., Gustafsson B., Piskunov N., Plez B., Reiners A. 2012, A&A 542, 330
• Phillips J.G., Davis S.P., Lindgren B., & Balfour W.J. 1987, ApJS 65, 721
• Piskunov et al. 1995, A&AS 112, 525 (VALD 1)
• Plez B. 1998, A&A 337, 495
• Stempels et al. 2001, ASP Conf. Ser. 223, 878, eds. R.J. Garcia Lopez, R. Rebolo, M.R. Zapaterio Osorio (VALD 2)