All-in-one tool to generate, and correctly drizzle, HST, JWST, and Roman PSFs.

Installation

To install: ```bash cd ~

git clone https://github.com/avapolzin/spike.git

cd spike

pip install .

` or bash pip install spike-psf ```

If you install from PyPI, you will also need to install DrizzlePac from the GitHub distribution.

To receive updates about the code, including notice of improvements and bug fixes, please fill out this form with your email.

Note that spike.psfgen.tinypsf and spike.psfgen.tinygillispsf require TinyTim for simulated PSFs. To use that module, please download TinyTim version 7.5 and follow the install instructions. Since that software is now unmaintained, refer to the STScI site for details and caveats.

If you plan to use the PSFEx empirical PSF modeling, that will similarly need to be downloaded from the GitHub repository and installed, as will SExtractor.

If you are using STPSF (formerly WebbPSF), you will need to install the relevant data and include it in your path. Instructions to do this are available here.

The jwst and romancal pipelines -- which house the tweak/resample steps for JWST and Roman -- require the setup of CRDSPATH and CRDSSERVER_URL environment variables. The amended version of the code also relies on crds, so it is necessary to set these environment variables according to the instructions here if you plan to use spike with JWST or Roman data.

If you install all of the optional dependencies described above, your shell's startup file will look something like:

``` bash

export TINYTIM="/path/to/tinytim-7.5" alias tiny1="$TINYTIM/tiny1" alias tiny2="$TINYTIM/tiny2" alias tiny3="$TINYTIM/tiny3"

export WEBBPSF_PATH="/path/to/webbpsf-data"

export STPSF_PATH="/path/to/STPSF-data"

export CRDSPATH="/path/to/crdscache/"

export CRDSSERVERURL="https://jwst-crds.stsci.edu"

export CRDSSERVERURL="https://roman-crds.stsci.edu"

```

Since both JWST and Roman CRDS servers may be used, these variables are defined directly within spike.psf.jwst and spike.psf.roman and do not need to be added to your startup file.

Additionally, spike is written to be backwards compatible with WebbPSF installations.

Getting Started

To get a drizzled PSF, only minimal inputs are required:

``` python

from spike import psf

acs_path = '/path/to/acs/data/'

psf.hst(imgdir = acspath, obj = 'M79', img_type = 'flc', inst = 'ACS', camera = 'WFC')

nircam_path = 'path/to/nircam/data/'

psf.jwst(imgdir = nircampath, obj = 'M79', img_type = 'cal', inst = 'NIRCam')

```

spike is intended to be fairly simple and can require as little as a working directory for images, the coordinates of an object of interest (where the PSF will be generated), the suffix used to identify relevant data (e.g., 'flc', crf', 'cal'), and the instrument used to take the data. For ACS and WFC3, a camera should also be specified. spike handles filter and detector/chip identification automatically, and the default parameters are sufficient to produce PSFs in most cases. The top-level functions spike.psf.hst, spike.psf.jwst, and spike.psf.roman also take a number of keyword arguments that allow for near-complete customization of the generated PSFs.

Ultimately, some of the other functions included in spike may be useful. For instance, the functions in spike.psfgen are methods to compute and save (to .fits) various model PSFs for a variety of telescopes/instruments which share similar syntax and required inputs and are callable from python directly. Similarly, spike.tools houses generic functions, which may be broadly applicable, including a python wrapper for SExtractor (not to be confused with sep), a utility to convert PSFEx .psf files to images, and a means of rewriting FITS files to an ASDF format. Please refer to spike-psf.readthedocs.io for details.

Testing spike

Since spike has utility for working with data, the most useful test of the code is to actually generate and drizzle PSFs from imaging. The code to generate Figures 1 and 2 from Polzin (2025) is in tests/test_outputs.py, which can be used to confirm the package works. Note that the input file structure is such that each instrument's data should be partitioned in its own directory, where all included data may be part of the final drizzled product.

An example file structure:

working_directory - testoutputs.py - *acswfcimaging* - wfc3uvis_imaging - wfpc2_imaging - nircam_imaging - miri_imaging - niriss_imaging

testoutputs.py includes the information for the datasets used and can also serve as a guide for testing other data. Note that different user inputs may be required based on data used (as for PSF generation and drizzling). Each run generates quite a few files, so I recommend moving testoutputs.py into its own directory rather than running it in the cloned spike one.

Similarly, one can test spike by running the code from the example notebooks.

Data-independent utilities included in spike can be tested via the scripts included in the "tests" directory here. To run these tests follow the below steps from your locally installed spike directory.

bash pip install pytest #necessary if pytest is not installed or in your working environment python -m pytest tests/tests.py

All tests should pass by default.

Issues and Contributing

If you encounter a bug, first check the documentation or the FAQ; if you don't find a solution there, please feel free to open an issue that details what you ran and what error you are encountering (or a PR with a fix). If you have a question, please feel free to email me at apolzin at uchicago dot edu.

If you would like to contribute to spike, either enhancing what already exists here or working to add features (as for other telescopes/PSF models), please make a pull request. If you are unsure of how your enhancement will work with the existing code, reach out and we can discuss it.