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SED-fitting python package for fitting evolved stars with DUSTY models
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README.md

Dusty-Evolved-Star-Kit

pypi Documentation Status Build Status arXiv paper Steve Goldman

The DESK is an SED-fitting python package for fitting data from evolved stars (photometry or spectra) with radiative transfer model grids. The package is currently in development and all contributions are welcomed. For current progress, see the Issues tab at the top of the page.

Input: A csv file with the first column as wavelength in um and second column as flux in Jy. To fit multiple csv files, put them in a directory, and use the directory name as the input.

Output: Two results files including the best fit model and corresponding stellar parameters, as well as an optional figure of the fit SED.

Available model grids: Several grids are already available upon installation. You can also specify the state-of-the-art dust growth models by Nanni et al. (2019), the 2D GRAMS model grid based on the 2DUST code, which are automatically downloaded and used when selected. New grids will also include the 1D radiation-hydrodynamic model grids from the DARWIN code.

A module for creating your own DUSTY grid is under development, but for now please email me (Dr. Steven Goldman) directly for grid requests or for help with the package.

Documentation

The documentation can be found on readthedocs.

Install Using Python

1). Install the package with the command pip install desk.

Using the DESK

2). Go to the directory where your target csv file (or target directory of files) is.

3). Use the command (without starting python)

desk fit --source='target_name.csv'

or if you have a folder of csv files

desk fit --source='folder_of_csvs'

additional options are:

desk fit --source='target_name.csv' --distance=50 --grid='H11-LMC'

These additional arguments are the distance (in kpc) and the grid of models you would like to use (options listed below). You can select 'oxygen' or 'carbon' to use the default models. To see other available grids use:

desk grids

This is an example of the output_sed.png file fitting three massive oxygen-rich AGB stars from the LMC. To produce individual figures subsequently run the command:

desk single_fig

Oxygen-Rich Model Grids

Oss-Orich-aringer (N=2,000): Uses warm silicates from Ossenkopf et al. 1992 and photospheric models from Aringer et al. 2016. Provides ranges in effective temperature (2600-3400 K: 200 K interval) inner dust temperature (600-1200K: 200 K interval) and optical depth (0.1 - 50: 100 spaced logarithmicly). Standard MRN grain size distribution from 0.005 - 0.25 microns.

Oss-Orich-bb (N=2,000): Same as Oss-Orich-aringer but using black bodies instead of the photospheric models.

Crystalline-20-bb (N=2,000): Same as Oss-Orich-bb but using 20% crystalline silicate grains from Jaeger et al. 1994.

corundum-20-bb (N=2,000): Same as Oss-Orich-bb but using 20% corundum grains from Begemann et al. 1997.

big-grain (N=2,000): Same as Oss-Orich-aringer but using a higher maximum dust grain size of 0.35.

fifth-iron (N=500): Same as Oss-Orich-aringer but with 20% iron grains from Henning et al. 1995, and an effective temperature of 3400 K.

half-iron (N=500): Same as Oss-Orich-aringer but with 50% iron grains from Henning et al. 1995, and an effective temperature of 3400 K.

one-fifth-carbon (N=500): Same as Oss-Orich-aringer but with 20% amorphous carbon grains from Zubko et al. 1996, and an effective temperature of 3400 K.

arnold-palmer (N=2,000): Same as Oss-Orich-aringer but with 50% amorphous carbon grains from Zubko et al. 1996.

Carbon-Rich Model Grids

Zubko-Crich-aringer (N=2,000): Same as Oss-Orich-aringer but with amorphous carbon grains from Zubko et al. 1996.

Zubko-Crich-bb (N=2,000): Same as Zubko-Crich-aringer but using black bodies instead of the photospheric models.

The dust growth model grids from Nanni et al. (2019)

H11-LMC (N=90,899): A carbon-rich grid for the LMC metallicity (1/2 solar) using optical constants from Hanner et al. (1988).

H11-SMC (N=91,058): A carbon-rich grid for the SMC metallicity (1/5 solar) using optical constants from Hanner et al. (1988).

J1000-LMC (N=85,392): A carbon-rich grid for the LMC metallicity (1/2 solar) using optical constants from Jager et al. (1998)

J1000-SMC (N=85,546): A carbon-rich grid for the SMC metallicity (1/5 solar) using optical constants from Jager et al. (1998)

The GRAMS model grids (Sargent et al. 2011; Srinivasan et al. 2011)

grams-carbon (N=12,244): A 2D carbon-rich grid using the 2DUST code for the LMC metallicity (1/2 solar) using optical constants from Zubko et al. 1996.

grams-oxygen (N=68,601): A 2D oxygen-rich grid using the 2DUST code for the LMC metallicity (1/2 solar) using optical constants from Ossenkopf et al. 1992.

- Warning: results uncertain outside of 20-150 kpc

Attribution

The method used is similar to that of Goldman et al. 2017; a more in-depth publication is in prep. If used please add the following to your acknowledgements:

This research has made use of the Dusty Evolved Star Kit (DESK; https://github.com/s-goldman/Dusty-Evolved-Star-Kit).

License

This project is Copyright (c) Dr. Steven Goldman and licensed under the terms of the BSD 3-Clause license.

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