From fd3e5a9df54547681666d5f66c9f9283e36dcae1 Mon Sep 17 00:00:00 2001 From: "Michael S. P. Kelley" Date: Tue, 16 Jan 2024 19:48:42 -0500 Subject: [PATCH] Document Afrho/Efrho.to_cross_section --- docs/sbpy/activity/dust.rst | 25 ++++++++++++++++++------- 1 file changed, 18 insertions(+), 7 deletions(-) diff --git a/docs/sbpy/activity/dust.rst b/docs/sbpy/activity/dust.rst index ef651820..ce3193d9 100644 --- a/docs/sbpy/activity/dust.rst +++ b/docs/sbpy/activity/dust.rst @@ -83,6 +83,13 @@ The `Afrho` class may be converted to a flux density, and the original value is >>> print(np.log10(f.value)) # doctest: +FLOAT_CMP -13.99 +`Afrho` may also be converted to geometric cross sectional area, given geometric albedo, photometric aperture, and observer-comet distance: + + >>> Ap = 0.05 # geometric albedo + >>> G = afrho.to_cross_section(Ap, aper, eph) + >>> print(G) # doctest: +FLOAT_CMP + 25763.15641363505 km2 + `Afrho` works seamlessly with `sbpy`'s spectral calibration framework (:ref:`sbpy-calib`) when the `astropy` affiliated package `synphot` is installed. The solar flux density (via `~sbpy.calib.solar_fluxd`) is not required, but instead the spectral wavelengths or the system transmission of the instrument and filter: .. doctest-requires:: synphot; astropy>=5.3 @@ -108,18 +115,22 @@ Reproduce the *εfρ* of 246P/NEAT from Kelley et al. (2013). .. doctest-requires:: synphot - >>> wave = [15.8, 22.3] * u.um - >>> fluxd = [25.75, 59.2] * u.mJy + >>> wave = 15.8 * u.um + >>> fluxd = 25.75 * u.mJy >>> aper = 11.1 * u.arcsec >>> eph = Ephem.from_dict({'rh': 4.28 * u.au, 'delta': 3.71 * u.au}) >>> efrho = Efrho.from_fluxd(wave, fluxd, aper, eph) - >>> for i in range(len(wave)): - ... print('{:5.1f} at {:.1f}'.format(efrho[i], wave[i])) # doctest: +FLOAT_CMP - 406.2 cm at 15.8 um - 427.9 cm at 22.3 um + >>> print(efrho) # doctest: +FLOAT_CMP + 396.71290996643665 cm + +Compare to 397.0 cm listed in Kelley et al. (2013). -Compare to 397.0 cm and 424.6 cm listed in Kelley et al. (2013). +`Efrho` may also be converted to geometric cross sectional area, given emissivity, photometric aperture, and observer-comet distance: + >>> epsilon = 0.95 # geometric albedo + >>> G = efrho.to_cross_section(epsilon, aper, eph) + >>> print(G) # doctest: +FLOAT_CMP + 391.83188076171695 km2 To/from magnitudes ^^^^^^^^^^^^^^^^^^