rot_int_cmj#
- excalibuhr.utils.rot_int_cmj(wave, flux, vsini, epsilon=0.6, nr=10, ntheta=100, dif=0.0)[source]#
Adapted from Carvalho & Johns-Krull (2023). See Adolfo1519/RotBroadInt
A routine to quickly rotationally broaden a spectrum in linear time. INPUTS: s - input spectrum w - wavelength scale of the input spectrum vsini (km/s) - projected rotational velocity
OUTPUT: ns - a rotationally broadened spectrum on the wavelength scale w OPTIONAL INPUTS: eps (default = 0.6) - the coefficient of the limb darkening law nr (default = 10) - the number of radial bins on the projected disk
ntheta (default = 100) - the number of azimuthal bins in the largest radial annulus note: the number of bins at each r is int(r*ntheta) where r < 1
dif (default = 0) - the differential rotation coefficient, applied according to the law Omeg(th)/Omeg(eq) = (1 - dif/2 - (dif/2) cos(2 th)). Dif = .675 nicely reproduces the law proposed by Smith, 1994, A&A, Vol. 287, p. 523-534, to unify WTTS and CTTS. Dif = .23 is similar to observed solar differential rotation. Note: the th in the above expression is the stellar co-latitude, not the same as the integration variable used below. This is a disk integration routine.