Switching from Legacy Software
This section provides basic switcher’s guide for those who are familar with
ASTROLIB PYSYNPHOT or IRAF SYNPHOT. This guide is not meant to be
all-inclusive; Therefore, not all legacy commands are listed here.
This is because a legacy command can be reproduced in several different ways
using synphot or has no equivalent implementation.
Naming convention used is the same as Quick Guide
Please contact STScI Help Desk if you have
any questions.
ASTROLIB Switcher Guide
Bandpass
| synphot |
ASTROLIB PYSYNPHOT |
|---|
| SpectralElement.from_file(filename) |
FileBandpass(filename) |
| SpectralElement.from_filter(filter) |
ObsBandpass(filter) |
| SpectralElement(Empirical1D,
points=wave, lookup_table=thru) |
ArrayBandpass(wavelength=wave,
throughput=thru) |
| SpectralElement(Box1D, amplitude=1,
x_0=mu, width=width) |
Box(mu, width) |
| bp.waveset |
bp.wave |
| bp(bp.waveset) |
bp.throughput |
| bp.taper() |
bp.taper() |
| bp.avgwave() |
bp.avgwave() |
| bp.tlambda() |
bp(bp.avgwave()) |
| bp.tpeak() |
bp.throughput.max() |
| bp.wpeak() |
bp.wave[bp.throughput ==
bp.throughput.max()] |
| bp.efficiency() |
bp.efficiency() |
| bp.equivwidth() |
bp.equivwidth() |
| bp.rectwidth() |
bp.rectwidth() |
| bp.rmswidth() |
bp.rmswidth() |
| bp.photbw() |
bp.photbw() |
| bp.pivot() |
bp.pivot() |
| bp.unit_response(area) |
bp.unit_response() |
| bp.emflx(area) |
bp.unit_response() * bp.equivwidth() /
bp(bp.avgwave()) |
| bp.check_overlap(sp) |
bp.check_overlap(sp) |
| bp.to_fits(filename) |
bp.writefits(filename) |
| bp.plot() |
matplotlib.pyplot.plot(bp.wave,
bp.throughput) |
Source Spectrum
| synphot |
ASTROLIB PYSYNPHOT |
|---|
| SourceSpectrum.from_file(filename) |
FileSpectrum(filename) |
| SourceSpectrum.from_vega() |
Vega |
| SourceSpectrum(Empirical1D,
points=wave, lookup_table=flux) |
ArraySpectrum(wave=wave, flux=flux) |
| SourceSpectrum(BlackBodyNorm1D,
temperature=teff) |
BlackBody(teff) |
| SourceSpectrum(ConstFlux1D,
amplitude=val*form) |
FlatSpectrum(val, fluxunits=form) |
| SourceSpectrum(PowerLawFlux1D,
amplitude=1*form, x_0=refval,
alpha=expon) |
Powerlaw(refval, expon,
fluxunits=form) |
| SourceSpectrum(GaussianFlux1D, mean=mu
, fwhm=fwhm, total_flux=flux) |
GaussianSource(flux, mu, fwhm,
fluxunits=form) |
| sp.waveset |
sp.wave |
| sp(sp.waveset) |
sp.flux |
| sp.taper() |
sp.taper() |
| sp.normalize(val*form, band=bp) |
sp.renorm(val, form, bp) |
| sp * extcurve |
sp * extcurve |
| SourceSpectrum(sp.model, z=z) |
sp.redshift(z) |
| sp.to_fits(filename) |
sp.writefits(filename) |
| sp.plot() |
matplotlib.pyplot.plot(sp.wave,
sp.flux) |
Observation
| synphot |
ASTROLIB PYSYNPHOT |
|---|
| Observation(sp, bp, binset=binset) |
Observation(sp, bp, binset=binset) |
| obs.waveset |
obs.wave |
| obs(obs.waveset) |
obs.flux |
| obs.binset |
obs.binwave |
| obs.binflux |
obs.binflux |
| obs(wave) |
obs.sample(wave, binned=False) |
| obs.sample_binned(wave) |
obs.sample(wave) |
| obs.effective_wavelength() |
obs.efflam() |
| obs.effstim(flux_unit=form) |
obs.effstim(form) |
| obs.countrate(area) |
obs.countrate() |
| obs.as_spectrum() |
obs.as_spectrum() |
| obs.as_spectrum().to_fits(filename) |
obs.writefits(filename) |
| obs.plot() |
matplotlib.pyplot.plot(obs.binwave,
obs.binflux) |
| obs.plot(binned=False) |
matplotlib.pyplot.plot(obs.wave,
obs.flux) |
Miscellaneous
| synphot |
ASTROLIB PYSYNPHOT |
|---|
| ReddeningLaw.from_extinction_model(law
).extinction_curve(val) |
Extinction(val, law) |
| generate_wavelengths(minwave=w1,
maxwave=w2, delta=dw) |
Waveset(w1, w2, dw) |
IRAF Switcher Guide
Bandpass
| synphot |
IRAF SYNPHOT |
|---|
| SpectralElement.from_file(filename) |
thru(filename) |
| SpectralElement.from_filter(filter) |
band(filter) |
| SpectralElement(Box1D, amplitude=1,
x_0=mu, width=width) |
box(mu, width) |
| bp.avgwave() |
bandpar bp photlist=avglam |
| bp.tlambda() |
bandpar bp photlist=tlambda |
| bp.tpeak() |
bandpar bp photlist=tpeak |
| bp.wpeak() |
bandpar bp photlist=wpeak |
| bp.efficiency() |
bandpar bp photlist=qtlam |
| bp.equivwidth() |
bandpar bp photlist=equvw |
| bp.rectwidth() |
bandpar bp photlist=rectw |
| bp.photbw() |
bandpar bp photlist=bandw |
| bp.fwhm() |
bandpar bp photlist=fwhm |
| bp.pivot() |
bandpar bp photlist=pivwv |
| bp.unit_response(area) |
bandpar bp photlist=uresp |
| bp.emflx(area) |
bandpar bp photlist=emflx |
| bp.to_fits(filename) |
calcband bp filename |
| bp.plot() |
plband bp |
Source Spectrum
| synphot |
IRAF SYNPHOT |
|---|
| SourceSpectrum.from_file(filename) |
spec(filename) |
| SourceSpectrum(BlackBodyNorm1D,
temperature=teff) |
bb(teff) |
| SourceSpectrum(ConstFlux1D,
amplitude=val*form) |
unit(val, form) |
| SourceSpectrum(PowerLawFlux1D,
amplitude=1*form, x_0=refval,
alpha=expon) |
pl(refval, expon, form) |
| SourceSpectrum(GaussianFlux1D, mean=mu
, fwhm=fwhm, total_flux=flux) |
em(mu, fwhm, flux, form) |
| sp.normalize(val*form, band=bp) |
rn(sp, bp, val, form) |
| SourceSpectrum(sp.model, z=z) |
z(sp, z) |
| sp.to_fits(filename) |
calcspec sp filename |
Observation
| synphot |
IRAF SYNPHOT |
|---|
| obs.effective_wavelength() |
calcphot bp sp flam func=’efflerg’ |
| obs.effstim(flux_unit=form) |
calcphot bp sp form |
| obs.countrate(area) |
calcphot bp sp counts |
| obs.plot(flux_unit=form) |
plspec bp sp form |
Miscellaneous
| synphot |
IRAF SYNPHOT |
|---|
| ReddeningLaw.from_extinction_model(law
).extinction_curve(val) |
ebmvx(val, law) |
| generate_wavelengths(minwave=w1,
maxwave=w2, delta=dw) |
genwave filename w1 w2 dw |
