Jieyu126 / SEDEX

SEDEX

SEDEX is a public pipeline written in Python to carry out SED fitting using MARCS and BOSZ spectral libraries. Based on its current configuration, SEDEX takes Gaia DR3 source ID, $T_{\rm{eff}}$, $\sigma_{T_{\rm{eff}}}$, $\textrm{log}g$, and $\sigma_{\textrm{log}g}$ as input, where $T_{\rm{eff}}$ is required to lift the $T_{\rm{eff}}-A_V$ degeneracy. SEDEX automatically downloads broadband photometry via Gaia archive. The current supported photometric systems are Gaia ( $G$, $G_{\rm{BP}}, G_{\rm{RP}}$), 2MASS ( $J, H, K_S$), ALLWISE ( $W1, W2, W3, W4$), Hipparcos ( $H_{P}$), Tycho2 ( $B_T, V_T$), SDSS ( $u, g, r, i, z$), Pan-STARRS1 ( $g, r, i, z, y$), APASS ( $V, B, g, r, i$), and SkyMapper ( $u, v, g, r, i, z$), consisting of 34 bandpasses.

The output of SEDEX includes bolometric flux, angular radius, extinction, luminosity, and radius. Extinction is a direct output, bolometric flux is calculated by integrating the best-fitting spectrum, luminosity is derived by combining bolometric flux and distance, radius is computed from luminosity and input $T_{\rm{eff}}$, and angular radius is inferred from radius and distance. More details can be found in Yu et al. 2022. Please cite this paper if you use it in your research.

Instructions on how to run SEDEX.

• Create a Gaia account and input your user name and password in the file $\texttt{inlist.py}$.
• Download MARCS (standard composition) and BOSZ (solar [C/M], resolution $R=20000$) spectral libraries.
• Prepare a list of targets in the file, $\texttt{Data/Input\_Fits/TOIs/UserInputData.csv}$, with these columns: starID, teff, tefferr, logg, loggerr, feh, feherr, Av, and Averr. Note that starID has to be Gaia DR3 source_id. Av and Averr can be NaN. The sample name, TOIs, can be optionally changed in the file $\texttt{inlist.py}$.
• Configure the inlist file, $\texttt{inlist.py}$. Suggest to use default values.
• Run $\texttt{submit.sh}$, if the single star mode is set, or run $\texttt{submit\_slurm.sh}$ for HPC, if the batch mode is set.
• Derived parameters are damped into this file: $\texttt{Data/Output\_Fits/TOIs/SEDFits/MARCS/Output\_SED\_Fits\_Final.csv}$. The figures of the Blackbody fitting and SED fitting are stored at $\texttt{Figures/TOIs/}$.