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LSF_ROTATE:
Create a 1-d convolution kernel to broaden a spectrum from a rotating star
Can be used to derive the broadening effect (line spread function; LSF) due to rotation on a synthetic stellar spectrum. Assumes constant limb darkening across the disk.
lsf = LSF_ROTATE(deltav, vsini, EPSILON=, VELGRID=)
deltaV - numeric scalar giving the step increment (in km/s) in the output rotation kernel. Vsini - the rotational velocity projected along the line of sight (km/s)
LSF - The convolution kernel vector for the specified rotational velocity. The number of points in LSF will be always be odd (the kernel is symmetric) and equal to either ceil(2*Vsini/deltav) or ceil(2*Vsini/deltav) +1 (whichever number is odd). LSF will always be of type FLOAT. To actually compute the broadening. the spectrum should be convolved with the rotational LSF.
Epsilon - numeric scalar giving the limb-darkening coefficient, default = 0.6 which is typical for photospheric lines. The specific intensity I at any angle theta from the specific intensity Icen at the center of the disk is given by: I = Icen*(1-epsilon*(1-cos(theta))
Velgrid - Vector with the same number of elements as LSF
(1) Plot the LSF for a star rotating at 90 km/s in both velocity space and for a central wavelength of 4300 A. Compute the LSF every 3 km/s IDL> lsf = lsf_rotate(3,90,velgrid=vel) ;LSF will contain 61 pts IDL> plot,vel,lsf ;Plot the LSF in velocity space IDL> wgrid = 4300*(1+vel/3e5) ;Speed of light = 3e5 km/s IDL> oplot,wgrid,lsf ;Plot in wavelength space
Adapted from rotin3.f in the SYNSPEC software of Hubeny & Lanz http://tlusty.gsfc.nasa.gov/index.html. Also see Eq. 17.12 in "The Observation and Analysis of Stellar Photospheres" by D. Gray (1992)
Written, W. Landsman November 2001
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