Description Usage Arguments Details Value Author(s) See Also
Read a one-dimensional spectrum from a fits file or ASCII data table and prepare for the kinematic analysis
1 2 3 |
file |
name of the fits file containing the spectrum. Filters are allowed, as understood by cfitsio. |
config |
name of a configuration file. Specifying this is enough
to read in a spectrum. Parameters than can be overridden explicitely
are |
noise |
name of a fits file containing the noise spectrum, or a
noise |
mask |
a mask in any format that can be read and converted by
|
order |
order of a polynomial fit to the continuum |
z |
redshift of the galaxy. Defaults to 0. |
lambda.lim |
wavelength range to be cut from the data cube. If
|
normalize |
logical. If TRUE, the spectrum is normalized to mean of
unity over the range defined by |
contsub |
logical. if TRUE a polynomial fit to the continuum will be subtracted from the spectrum |
contdiv |
logical. If TRUE, the spectrum will be divided by a polynomial fit to the continuum |
verbose |
logical. If TRUE, give some progress report. |
object |
an optional name of the object |
A one-dimensional spectrum is read from a file and returned in
the form of a list. Optionally, a noise vector is added. The spectrum
is deredshifted and optionally a polynomial fit to the continuum is
subtracted from the spectrum. The input file can be either a fits file
or an ASCII file in the format of a data table with at least columns
lambda
and value
.
a list containing the following elements:
lambda |
the wavelength values of the deredshifted spectrum |
value |
the original values of the spectrum |
noise |
the estimated noise for each wavelength pixel |
mask |
a logical vector with |
contsub |
(optional) the values of the spectrum after subtraction of a continuum fit |
contdiv |
(optional) the values of the spectrum after division by a continuum fit |
name |
the name of the input fits file |
object |
the name of the object |
Oliver Czoske
prepare.template
, link{prepare.cube}
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