Next steps#
No plots, just exposure times#
You can also calculate the exposure time required to obtain a given S/N using
the signal_to_noise_to_exp_time
function. For example - how many
seconds must one expose ARCES on a V=12 mag M0V star to get a S/N of 30 at the
wavelength of H-alpha:
from arcesetc import signal_to_noise_to_exp_time
import astropy.units as u
sptype = 'M0V'
wavelength = 6562 * u.Angstrom
signal_to_noise = 30
V = 12
print(signal_to_noise_to_exp_time(sptype, wavelength, V, signal_to_noise))
This returns 642.11444 s
, a Quantity
object containing the
required exposure time.
Available spectral types#
You can see which spectral types are available with the
available_sptypes
function.
Note
At present, the best coverage is for mid-F through mid-M type main sequence stars, with some M giants.
Here’s a color-magnitude diagram of the stars presently available in arcesetc
:
How it works#
We estimate the count rates for stars as a function of wavelength by fitting
15th-order polynomials to each spectral order of real observations of a star of
each spectral type. These polynomial coefficients and some wavelength metadata
are stored in an HDF5 archive for compactness and ease of reconstruction. Then
upon calling arcesetc
, the archive is opened and the spectral order closest
to the wavelength of interest is reconstructed from the polynomial
coefficients, for a star of the closest available spectral type to the one
requested.
Warning
arcesetc
doesn’t know anything about saturation.
Run the tests#
If you’re contributing to arcesetc
, you can check that your updates don’t
break the API by running the tests like this in the source directory:
tox -e test
If the tests pass, you’re ready to submit a pull request!