Description Usage Arguments Details Value Author(s) See Also
This function is a wrapper function, it calls
fit.spectrum
for every spectrum in a VIMOS IFU data
cube.
1 2 3 4 |
config |
name of a file or list containing relevant data on the object on which the kinematic analysis is to be performed |
galspec |
(optional) a list of galaxy spectra, all on the same
wavelength vector. This would be read in from a VIMOS cube with
|
template |
(optional) an object of class |
LOSVD |
Shape of the LOSVD to be fit to the spectrum. Defaults to Gaussian but can also be set to a Gauss-Hermite series, to order 4. |
mask |
a data.frame with two columns |
output |
the name of a file to which the resulting fit will be
written by |
errors |
Number of Monte Carlo simulations that will be performed for each spectrum in the cube to give an estimate of the error distribution; defaults to zero |
SN.lim |
Only spectra in the cube which have a signal-to-noise
ratio larger than this value will be analysed by
|
dv |
velocity step on which the template spectrum will be initially sampled; defaults to 25 km/sec |
verbose |
|
sigma.max |
Maximum allowed value for the velocity dispersion, defaults to 1000 km/s. This gives in principle a constrained optimization, although the best fit should not be affected. |
normalize |
Normalization factor for the data cube, defaults to
|
... |
Further parameters to be passed to
|
Beware of running too many error realizations, this takes a hell of a long time.
An object of class kinmap
obtained from fit.spectrum
with simple=TRUE
. If output
is
given, the result will be written directly to a file in the form of a
data.frame
.
v, sig, gof, h3, h4 |
The best fitting values for velocity and
velocity dispersion, and the corresponding value of the
|
v1, v2 |
first and second velocity moments of the best-fitting LOSVD |
dv.low, dv.high, dsig.low, dsig.high,... |
If |
SN, level, noise |
The signal-to-noise, level and noise for the galaxy spectrum. |
rms |
The root-mean-square residuals of the best fit; this can be compared to noise |
L, M |
coordinates of the fibre in the data cube |
template, sptype, FeH, logg, Teff |
some data on the template used |
Oliver Czoske
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