Data

Here I aim to make available some data (some published, some unpublished) which might be of use to someone.

Index:

Atomic data
- Collisional broadening by hydrogen
- Inelastic electron collision data
- Inelastic hydrogen collision data
Observed Spectra
- S4N database
Theoretical spectra
- Hydrogen line grids
Stellar data
- HERES survey

Atomic data

Collisional broadening by hydrogen

Data for 4891 spectral lines between 2300 and 13000 Angstroms of elements from Li to Ni: lines, description
These data were published in Barklem et al (2000).
Data for Cr II lines: lines, levels
Data for Fe II lines: lines, levels
The data for Fe II was published in Barklem & Aspelund-Johansson (2005). The Cr II data was calculated in 2007 due to a request and used in Sobeck et al (2007). The calculations used the method described in Barklem & Aspelund-Johansson (2005), so if you use the Cr II data you can cite that paper for the method.

A general description of how to use Anstee, Barklem & O'Mara theory data is given here. A general program for interpolating data for broadening of lines neutral atoms from precomputed tables is given here

Inelastic electron collision data

Data for O + e inelastic collisions: rate coefficients, levels
These data were published in Barklem (2007), though here I have extended the temperature range up to 100000 K, and included the data for all 19 spectroscopic states as only the data for the lowest 7 were included explicitly in the paper.

Inelastic hydrogen collision data

Data for Li + H inelastic collisions: rate coefficients
These data were published in Barklem et al (2003) and are based on cross sections published in Belyaev & Barklem (2003).
Data for Na + H inelastic collisions: rate coefficients
These data were published in Barklem et al (2010) and are based on cross sections published in Belyaev et al (2010).

Observed spectra

S4N

S4N Database
High resolution observed optical spectra for 118 nearby stars from the Spectroscopic Survey of Stars in the Solar Neighbourhood project, Allende Prieto et al (2004)

Theoretical spectra

Hydrogen line grids

F,G, and K dwarfs,
Teff: 4400 to 7500 K, logg: 3.4 to 5.0, [Fe/H]: -3.0 to +0.5, microturbulence: 1.5 km/s :
Halpha, Hbeta, Hgamma, Hdelta (each file approx 10 Mb)
F,G, and K dwarfs, with alpha-enhancement
Teff: 4400 to 7500 K, logg: 3.4 to 5.0, [Fe/H]: -3.0 to +0.5, microturbulence: 1.5 km/s (with alpha enhancement of +0.4 dex):
Halpha, Hbeta, Hgamma, Hdelta (each file approx 10 Mb)
G and K giants,
Teff: 4400 to 6000 K, logg: 1.0 to 3.4, [Fe/H]: -3.0 to +0.5, microturbulence: 1.5 km/s:
Halpha, Hbeta, Hgamma, Hdelta (each file approx 8 Mb)
Metal-poor giants, with alpha-enhancement
Teff: 4500 to 5500 K, logg: 1.0 to 3.0, [Fe/H]: -3.0 to -2.0, microturbulence: 1.5 km/s (with alpha enhancement of +0.4 dex):
Halpha, Hbeta, Hgamma, Hdelta (each file approx 1.3 Mb)
Here is a short IDL routine to read the profiles. The profiles are labelled with files names of the form:
alf_synth_t6100g4.65m-0.25x1.5.prf
where:
alf is H alpha
synth is the line formation code used
6100 is Teff
4.65 is logg
-0.25 is metallicity
1.5 is the microturbulence in the model atmosphere calculation.
These are hydrogen line profiles calculated as described in Barklem et al (2002) (i.e. 1D, LTE, 1997 epoch MARCS, Stehle + BPO) using self-broadening theory developed in Barklem et al (2000). MLT parameters alpha = 0.5 and y = 0.5 are used in all these model calculations. Note the line formation calculation includes no micro- or macroturbulence, but this has no effect on the wings. The line cores are not expected to form in the photosphere or in anything close to LTE, and thus are not reliable and should not be used for any interpretation of observations.
The codes used for these line formation calculations are available here.

Stellar data

HERES survey

These are the data obtained in the HERES survey Barklem et al (2005). Table 1 is the stellar sample (coordinates and radial velocities) and Table 2 the derived stellar properties (parameters, chemical abundances).

I have also derived upper limits for the sample in two ways. I provide both cases in case they are useful, but would recommend using the second file.

The first gives the abundance at which the most important line in the spectrum may be detected at 3 sigma significance level, and thus is an upper limit if the element is undetected in the HERES II paper. Only one case has no data (HE1256-0228 for Y) in the table (it has a NaN in fact). This is because the Y line I use for the upper limit is near the blue cutoff for the spectra, and in this particular case there are no observations at this wavelength (probably due to a large radial velocity of the star). But this is not an issue anyway as Y is detected in this star in any case.
However, there is a minor complication. In the automated method, sometimes lines are cut if they lie close to a Balmer line or are suspected of being affected by some type of artefact (like a cosmic ray hit). Thus, there is a chance that the line used to get the upper limit was not in fact used in the spectrum analysis. The value in the first file is likely to be underestimated in such a case. Anyway, I provide a second version, where cases where the line was cut from the analysis are not included (they have NaN as the result). Note, this is naturally only an issue if there is no detection; so for example it happens a lot for Co (due to the line being in a Balmer line wing) but Co is almost always detected anyway.