Chemical Elements as Tracers of the Evolution of the Cosmos - Infrastructures for Nuclear Astrophysics

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Stellar Analysis Pipeline

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User info (optional)

User name

Email address

Instr. specs & Source (optional)

Instrumental broadening

SNR

Gaia DR3 ID

Vrad

Stellar parameters

Teff

logg

monh

Vmic

Vmac

Vsini

Checked: Parameter p will be derived by SME using an initial guess provided through the textbox. Unchecked: p is fixed to the value provided in the textbox.

Use MCMC

When activated, the best-fit values and uncertainties will be derived via MCMC. This may lead to very long runtimes (more than several hours).

References

Solar ref. composition

Asplund 2021
Asplund 2009
Grevesse 2007
Lodders 2003
User defined

Linelist

Gaia-ESO
Gaia-ESO (Y,Y|U)
VALD (F-type stars)
VALD (G-type stars)
VALD (K-type stars)
VALD (red clump)

Derive abundance

Select elements

Reported abundances are on the "12+log-epsilon" scale, i.e. log10 of the fraction of nuclei of the element in any form relative to the number of hydrogen in any form plus an offset of 12. For the Sun, the abundance values of H, He, and Li are approximately 12, 10.9, and 1.05.

Lines for abundance measurement

If stellar parameters (Teff, logg and monh) are fixed, abundances may be derived using only the lines selected below.

Limit wavelength range from to Å

NLTE (Li, Mg, Na, O, Si, Ba, Ca, Fe, Ti)

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This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 101008324 (ChETEC-INFRA).