OII.model: Collection of functions to create an OII map from VIMOS data

Description Usage Arguments Details Value Note Author(s) References See Also

View source: R/OII-model.R

Description

These functions determine the strength of the [OII] doublet across a VIMOS/IFU data cube by fitting a double Gaussian model to the lines. Depending on the signal-to-noise ratio of the individual spectra the template fit to the entire spectrum is subtracted before fitting [OII].

Usage

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OII.model.map(config.file, cube.fit, galspec, template,
              plot=FALSE, m1=NULL, m2=NULL, normalize=1e-18, ...)
OII.model(lambda, m1 = 5277, m2 = 5281.5, s1 = 1.2, s2 = 1.2, a.rel = 1.5)
OII.fit(galaxy, template, spec.fit, model, plot=FALSE, ...)
OII.gof(p=c(1), y, y.mod)

Arguments

config.file

name of list or file containing configuration data pertinent to the galaxy to be analysed

cube.fit

a data.frame containing the results of kinematic fits to the data cube, as obtained with fit.cube

spec.fit

a data.frame (with one row) or list containing the results from a kinematic fit to a single spectrum. This can be a single row from cube.fit or the results from fit.spectrum. The minimum requirements are components v, sigma and SN.

galspec

(optional) a list of galaxy spectra, all on the same wavelength vector. This would be read in from a VIMOS cube with prepare.cube. If missing, the name of the data cube is taken from config

galaxy

a single galaxy spectrum on which the [OII] line strength is to be determined

template

(optional) an object of class spectrum containing the stellar template spectrum. If missing, the name of the template file is taken from config

plot

(logical) If TRUE, OII.model.map displays the [OII] map; OII.fit displays the spectrum and the best double Gaussian fit if the function is called directly.

m1, m2, s1, s2, a.rel

central wavelengths, dispersions and relative strength of the Gaussians describing the two components of the [OII] doublet model.

model

(optional) a model for the [OII] doublet as returned by OII.model. OII.fit determines the scaling needed to match this model to the actual [OII] lines.

normalize

normalization constant used to bring the spectral values to order unity

lambda

wavelength vector on which the [OII] model is built

p

starting value for the scaling of the model

y, y.mod

the data and model vectors used to compute the goodness of fit

...

parameters that are passed to build.model, i.e. affecting the kinematic model

Details

The function OII.model.map is the one typically used directly. The other functions (with the possible exception of OII.fit) are used internally to compute the [OII] model, the goodness-of-fit for a given model, and to optimize the fit.

Value

OII.model.map returns a data.frame containing positions L and M the signal-to-noise ratio of the spectrum, SN, and the strength of the [OII] lines, Flux. This can be visualized with plot.kinmap

OII.fit returns the same values in the shape of a list and for a single spectrum.

OII.model returns a spectrum, i.e. a list with lambda and value.

OII.gof returns a number, the sum of squared differences between data and model.

Note

THIS IS NOT QUITE FINISHED YET!

Author(s)

Oliver Czoske

References

The procedure follows an idea described by Bolton \& Burles (2008).

See Also

fit.cube, build.model, plot.kinmap


oczoske/slacR documentation built on May 20, 2019, 8:23 p.m.