PySTELLA

IMPORTANT: the package is under heavy development. Keep this in mind if you want to use it on your research.

Command shell

Run the script "PATH-to-PySTELLA/pystella.py" in the directory with models. See help if needed.

Load the flux from ph-files and convert them to the bands

Usage: ubv.py [params]

• -b bands:shift: string, default: U-B-V-R-I, for example U-B-V-R-I-u-g-i-r-z-UVW1-UVW2. shift: to move lc along y-axe (minus is '_', for example -b R:2-V-I:_4-B:5
• -i <model-name OR pattern, like 'R450'>. Example: cat_R450_M15_Ni007_E7
• -p , default: ./
• -e <extinction, E(B-V)> is used to define A_nu, default: 0
• -c [lcobs:fname:marker:dt:dm, velobs:fname:marker:dt:vnorm(1e8), popov[:R:M:E[FOE]:Mni], lcobssm as lcobs, but for sm-format data-files]. You can add parameters in format func:params
• -d [pc]. Default: 10 pc
• -g <single, grid, gridm, gridl> Select plot view. single [default] = all models in one figure, grid = for each band separate figure.
• -o <is_axes_right>. Default: empty string
• -m . Default: None, used for grav lens
• -q turn off quiet mode: print info and additional plots
• -t plot time points
• -s without extension. Save plot to pdf-file. Default: ubv_.pdf
• -x xbeg:xend - xlim, ex: 0:12. Default: None, used all days.
• -y ybeg:yend - ylim, ex: 26:21. Default: None, used top-magnitude+-5.
• -v <swd OR ttres[ttresold]> - plot model velocities computed from swd OR tt-res files[ttresold for old res format].
• -w write magnitudes to out-file. Use '1' for the default name of out-file
• -z . Default: 0
• --dt=<t_diff> time difference between two spectra
• --curve-old - use old procedure
• --curve-tt - take curves from tt-file: UBVRI+bol
• -l write plot label
• -h print usage

Available bands:

• AtlasC AtlasO
• Bbes Ibes Rbes Ubes Vbes
• F105W F125W F140W F160W F435W F606W F814W
• GaiaG
• HSCY HSCg HSCi HSCr HSCz
• KaitB KaitI KaitR KaitU KaitV Kepler
• LcoH LcoJ LcoK Lum
• PS1g PS1i PS1r PS1w PS1y PS1z
• gSdss iSdss rSdss uSdss zSdss SwiftB SwiftU SwiftV
• USNO40g USNO40i USNO40r USNO40u USNO40z UVM2 UVW1 UVW2
• bol bolq
• massH massJ massK
• ubvri

Available aliases of bands:

• U => Ubes B => Bbes V => Vbes R => Rbes I => Ibes
• g => gSdss r => rSdss i => iSdss u => uSdss z => zSdss
• J => massJ H => massH K => massK

Run

Run script for all *.ph-files in the DIR:

 find DIR  -name "*.ph" | sed -r 's/\.ph$//' | while read fn; do ./ubv.py -i $(basename  $fn)  -d $(dirname $fn) -s; done

also the same could be done with key '-p' without model's name.

Install:

 git clone https://github.com/baklanovp/pystella.git
 cd pystella

Create conda environment:

conda env create -f environment.yml
conda activate nb

and work

 ./pystella.py

OR

 ./ubv.py [params]

OR

 ipython
ipython> import sys
ipython> sys.path.append('path-to-root-pystella')
ipython> import pystella as ps

Requirements

 pip3 install -r requirements.txt

OR manually

To plot light curves [ubv] and shock wave details [swd]

 apt-get install python3
 apt-get install python3-numpy python3-scipy
 apt-get install python3-matplotlib
??? apt-get install python3-tk

To fit observations

 apt-get install -y python3-pip
 pip3 install emcee
 pip3 install cython
 pip3 install gptools
 pip3 install corner

Tests

 python3 -m unittest discover ./tests/

Testing can take a long time.

Some tests plot the comparison charts, they must be closed to continue the work. It is not necessary that all tests show OK. Some of them are non-working yet.

Citing PySTELLA

Please add some form of acknowledgement that you used this code.

Acknowledgments:

Some of the passbands was taken from  SNPY (see http://csp.obs.carnegiescience.edu/data/snpy/),
SnCosmost (see https://github.com/srodney/sncosmost), and http://svo2.cab.inta-csic.es/svo/theory/fps3/index.php.