jwst.py ¶
A Python interface for simulating time-series filter photometry with the James Webb Space Telescope (JWST).
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class
planetplanet.detect.jwst.Filter(name=None, wl=None, throughput=None, dwl=None, eff_wl=None, eff_dwl=None)¶ A photometruc filter class. This is an interface for filter photometry calculations.
Parameters: - name (str) – Name of the filter
- wl (array_like) – Wavelength grid for filter [\(\mu \mathrm{m}\)]
- throughput (array_like) – Filter throughput
- dwl (array_like) – Wavelength width grid for filter [\(\mu \mathrm{m}\)]
- eff_wl (float) – Effective filter wavelenth [\(\mu \mathrm{m}\)]
- eff_dwl (float) – Effective filter width [\(\mu \mathrm{m}\)]
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compute_lightcurve(time, flux, continuum, lam, stack=1, atel=25.0, thermal=True, time_hr=None, flux_hr=None, quiet=False)¶ Computes an observed lightcurve in the
Filter().Parameters: - time (array_like) – Time grid [days]
- flux (array_like) – Observed flux grid (time by lam) [\(\mathrm{W/m}^2 / \mu \mathrm{m}\)]
- continuum (array_like) – Observed continuum flux grid (no occultations, shape time by lam) [\(\mathrm{W/m}^2 / \mu \mathrm{m}\)]
- lam (array_like) – Wavelength [\(\mu \mathrm{m}\)]
- stack (int) – Number of exposures to stack. Default 1
- atel (float) – Telescope collecting area [\(\mathrm{m}^2\)]. Default 25
- thermal (bool) – Compute thermal noise. Default
True - time_hr (array_like) – High-res time grid [Days]. Default
None - flux_hr (array_like) – High-res flux grid. Default
None
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convolve(lam, flux)¶ Convolve flux with normalized filter throughput.
Parameters: - lam (array_like) – High-res wavelength grid [\(\mu \mathrm{m}\)]
- flux (array_like) – High-res flux grid [\(\mathrm{W/m}^2 / \mu \mathrm{m}\)]
Returns array_like F: Flux convolved with normalized throughput
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photon_rate(lam, flux, atel=25.0, dlam=None)¶ Compute the photon count rate registered by the detector.
Parameters: - lam (array_like) – High-res wavelengths [\(\mu \mathrm{m}\)]
- flux (array_like) – Spectral flux density [\(\mathrm{W/m}^2 / \mu \mathrm{m}\)]
- atel (float) – Telescope collecting area [\(\mathrm{m}^2\)]. Default is 25
- dlam (array_like) – Delta-wavelength grid. Default is
Noneand is calculated
Returns array_like cphot: Photon count rate [\(\mathrm{s}^{-1}\)]
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plot(ax=None)¶ Plots the filter throughput curve.
Parameters: ax ( axis) – An axis instance
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planetplanet.detect.jwst.estimate_eclipse_snr(tint=2184.0, nout=4.0, lammin=1.0, lammax=30.0, Nlam=10000, Tstar=2560.0, Tplan=400.0, Rs=0.12, Rp=1.086, d=12.2, atel=25.0, verbose=True, plot=True, thermal=True, filters='MIRI')¶ Estimate the signal-to-noise on the detection of secondary eclipses in JWST/MIRI photometric filters.
Parameters: - tint (float) – Exposure time [s]. Default 36.4*60.
- nout (float) – Out-of-transit time observed [transit durations]. Default 4
- lammin (float) – Wavelength minimum [\(\mu \mathrm{m}\)]. Default 1.0
- lammax (float) – Wavelength maximum [\(\mu \mathrm{m}\)]. Default 30.0
- Nlam (int) – Number of wavelengths. Default 10000
- Tstar (float) – Stellar effective temperature [K]. Default 2560
- Tplan (float) – Planet equilibrium temperature [K]. Default 400
- Rs (float) – Stellar radius [solar radii]. Default 0.12
- Rp (float) – Planet radius [Earth radii]. Default 1.086
- d (float) – System distance [pc]. Default 12.2
- atel (float) – Telescope collecting area [\(\mathrm{m}^2\)]. Default 25
- verbose – Print things. Default True
- plot – Make a plot. Detault True
- thermal – Include thermal noise. Default True
- filters (str or list of
Filter()objects) – User provided filter names or list of filters. Default MIRI
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planetplanet.detect.jwst.create_tophat_filter(lammin, lammax, dlam=0.1, Tput=0.3, name='custom')¶ Create a tophat
Filter()Parameters: - lammin (float) – Wavelength minimum [\(\mu \mathrm{m}\)]
- lammax (float) – Wavelength maximum [\(\mu \mathrm{m}\)]
- dlam (float) – Wavelength resolution [\(\mu \mathrm{m}\)]. Default 0.1
- Tput (float) – Filter throughput. Default 0.3
- name (str) – Name of filter. Default “custom”
Returns filt: New custom tophat
Filter()object