v0.13.0

Installing

• ECLIPSE is now on PyPI as eclipse: pip install eclipse. pip install solarc-eclipse stops with a message saying so, and versions up to 0.12.1 still install under the old name when the version is given. (#189)
• The package is imported as eclipse, the name of its command. import euvst_response still works, with a warning. (#174)

New

• A full-CCD frame of the SW camera, with every line in the band and the continuum, made by full_ccd_frame and written by write_full_frame. (#157, #162, #170, #188)
• synthesise-spectra --continuum adds the free-free, free-bound and two-photon continuum. (#156)
• The SW PSF includes the resolution budget's blur, chosen with telescope.resolution_budget, with telescope.field_of_view and telescope.pointing_jitter. (#165)
• simulation.slit_mask blocks the light beyond the ends of the slit and behind its fiducials. (#164)
• The DN fits weight each pixel by its uncertainty, and the photon fits use the Poisson likelihood; fitting.weighted: false gives the unweighted fits. (#152)
• simulation.readout_dark_current counts the dark current collected while the CCD is cleared and read out, and is on by default for SWC. (#191)
• simulation.focal_plane_dispersion takes the pixels' width in wavelength from the SW focal plane where the line lands. (#193)
• --integration-axis takes a sign, such as -x, to look from either side of the box. (#146)
• Instrument values that were fixed in the code are settings, such as the detector's Fano factor and pair energy, and the SW camera's read-out timing and focal plane. (#147, #173)
• Spectra with NaN pixels are fitted on their finite pixels. (#172, #178)
• Line lookups are cached, which makes syntheses of many lines much faster. (#149)

Replaced, and still working with a warning

• The import name euvst_response, now eclipse. (#174)
• detector._dark_current_293k, now detector.dark_current_293k. (#173)

Documentation

• "Where the settings come from" gives the source of each instrument default, and is checked against the code. (#169, #180)
• "The instrument model" describes what ECLIPSE models, apart from how to run it, and the reference pages are gathered together. (#195)

Changes to output

• Output can differ from v0.12.1 for the same input, so results made with earlier versions should be regenerated. The largest changes come from the weighted fits (#152), the resolution budget's blur in the SW PSF (#165), and, for a single line of known intensity with the PSF on, the blur applied before the line is laid onto the pixels (#190).