scopesim.source.source_templates module

scopesim.source.source_templates.ab_spectrum(mag=0)

scopesim.source.source_templates.empty_sky(flux=0)

Returns an empty source so that instrumental fluxes can be simulated

Returns:

skySource

scopesim.source.source_templates.st_spectrum(mag=0)

scopesim.source.source_templates.star(x=0, y=0, flux=0)

Source object for a single star in either vega, AB magnitudes, or Jansky

The star is associated with the reference spectrum for each photometric system, therefore a reference wavelength or filter does not need to be given

Parameters:

x, yfloat

[arcsec] position from centre of field of view

fluxfloat

[vega mag, AB mag, Jy] Stellar brightness

Returns:

srcSource

A source object with a single entry table field and a reference spectrum

scopesim.source.source_templates.star_field(n, mmin, mmax, width, height=None, use_grid=False)

Creates a super basic field of stars with random positions and brightnesses

Parameters:

nint

number of stars

mmin, mmaxfloat, astropy.Quantity

[mag, ABmag, Jy] min and max magnitudes/fluxes of the population stars. If floats, then assumed Quantity is vega magnitudes

widthfloat

[arcsec] width of region to put stars in

heightfloat, optional

[arcsec] if None, then height=width

use_gridbool, optional

Place stars randomly or on a grid

Returns:

starsscopesim.Source object

A Source object with a field of stars that can be fed into the method: OpticalTrain.observe()

See also

OpticalTrain.observe

OpticalTrain.readout

scopesim.source.source_templates.uniform_illumination(xs, ys, pixel_scale, flux=None, spectrum=None)

Return a Source for a uniformly illuminated area

Parameters:

xs, yslist of float

[arcsec] min and max extent of each dimension relative to FOV centre E.g. xs=[-1, 1], ys=[5, 5.5]

pixel_scalefloat

[arcsec]

fluxastropy.Quantity

[mag, ABMag, Jy] Flux per arcsecond of the Source

Returns:

srcscopesim.Source

Examples

A 200x200 uniform illumination Source at 1 Jy/arcsec2

src = uniform_illumination(xs=[-1,1], ys=[-1, 1],
                           pixel_scale=0.01, flux=1*u.Jy)

A source that extends just past the MICADO 15” slit dimensions with a flux of 10 mag/arcsec2

src = uniform_illumination(xs=[-8, 8], ys=[-0.03, 0.03],
                           pixel_scale=0.004, flux=10*u.mag)

Using a self made frequency-comb spectrum with 1 Jy lines ever 0.1µm

import numpy as np
from astropy import units as u
from synphot import SourceSpectrum, Empirical1D

wave = np.arange(0.7, 2.5, 0.001) * u.um
flux = np.zeros(len(wave))
flux[::100] = 1 * u.Jy
spec = SourceSpectrum(Empirical1D, points=wave, lookup_table=flux)

src = uniform_illumination(xs=[-8, 8], ys=[-0.03, 0.03],
                           pixel_scale=0.004, spectrum=spec)

scopesim.source.source_templates.uniform_source(sp=None, extent=60)

Simplified form of scopesim_templates.misc.uniform_source, mostly intended for testing

This function creates an image with extend^2 pixels with pixel size of 1 arcsec^2 so provided amplitudes are in flux or magnitudes per arcsec^2

It accepts any synphot.SourceSpectrum compatible object

spsynphot.SourceSpectrum

defaults to vega_spectrum() with magnitude 0 mag/arcsec2

extentint, default 60

extension of the field in arcsec, will always produce a square field. Default value produces a field of 60x60 arcsec

scopesim.source.source_templates.vega_spectrum(mag=0)