ALFA: automated line fitting algorithm: manual (v2.0.50)
alfa − automated line fitting algorithm
alfa [OPTION] [VALUE]... [FILE]
alfa rapidly fits emission line spectra, using a genetic algorithm to optimise fitting parameters. It is intended to be entirely automated, but while the default values should work well in many situations, a good fit to your observed spectrum may require some adjustments to the input parameters. It is optimised for optical spectra, but can be applied to any wavelength range if a suitable line catalogue is provided.
alfa reads one dimensional spectra in either plain text or FITS format. Plain text input should consist of two columns, giving wavelength and flux. It can also read data cubes and row-stacked spectra in FITS format. Results are written out in plain text, to files containing the fit (total fit, continuum-subtracted original, continuum, sky lines and residuals), and the line flux measurements.
−b, −−bad-data [REAL]
If all values in a spectrum are below the value specified, alfa will not fit it. Most useful for avoiding wasting time on low signal regions of data cubes.
Prints out the bibliographic details of the paper to cite if you use alfa in your research.
Sums all spectra in multi-dimensional FITS files into a single spectrum. Spectra whose peak value is below any value specified with the --bad-data option are excluded. --collapse has no effect on 1D data.
−cw, −−continuum−window [INTEGER]
ALFA’s continuum fitting takes the 25th percentile of flux values in a moving window as representative of the continuum level. This option can be used to set the size of the window. The value must be an odd integer. Default: 101
−dl, −−detection-limit [REAL]
Sets the factor by which a line’s flux must exceed the locally estimated noise level for it to be considered a detection. Default: 3.0
−el, −−exclude-line [REAL]
When reading in the line catalogues, any wavelengths indicated with this option will be ignored. For example, if H alpha were saturated, it could be excluded from the fit with --exclude-line 6562.77. Any number of lines can be excluded by repeating the option with the appropriate wavelengths.
−fc, −−flux-column [INTEGER]
When reading FITS tables, this option can be used to specify in which table column the flux values are. For any other file type it will have no effect. Default: 2
−g, −−generations [INTEGER]
The number of generations used in the genetic algorithm. Default: 500
−n, −−normalise [VALUE]
Normalise to Hb=100 assuming that F(Hb)=VALUE. If VALUE is zero, no normalisation is applied. If this option is not specified, fluxes are normalised using the measured value of Hb if it is detected, and not normalised otherwise.
In case the spectrum you are fitting is already continuum subtracted, setting this option skips alfa’s continuum fitting.
alfa’s default behaviour is that it will not overwrite any pre-existing output file. If this option is specified, then the output file will be overwritten.
−o, −−output−dir [DIRECTORY]
The directory in which to put the output files. Default: current working directory.
−of, −−output-format [VALUE]
The format of the output files. Valid values are text, csv, fits, latex. If you are using alfa in conjunction with neat, plain text and fits formats can currently be read in. Default: text
−pr, −−pressure [REAL]
The fraction of the population retained from each generation. The product of the pressure and the population size should be an integer. Default: 0.3
−ps, −−populationsize [INTEGER]
The size of the population used in the genetic algorithm. Default: 30
−rb, −−rebin [INTEGER]
Rebin the input spectrum by the specified factor. Useful for high resolution spectra where line profiles are not instrumental but kinematic. This option is currently only implemented for 1d spectra.
−rg, −−resolution−guess [VALUE]
Initial guess for the resolution [lambda/delta lambda]. Default: estimated using the sampling of the input spectrum, assuming that it is Nyquist sampled.
−rtol1, −−resolution−tolerance−1 [VALUE]
Variation allowed in resolution in first pass. Default: equal to 0.9 x resolution guess.
−rtol2, −−resolution−tolerance−2 [VALUE]
Variation allowed in resolution in second pass. Default: 500.
−skyc, --sky-catalogue; −sc, --strong-catalogue; −dc, --deep-catalogue [FILENAME]
The files containing the line catalogues to be used for the removal of sky lines, the estimation of velocity and resolution, and the full line fitting. The default catalogues are stored in /usr/share/alfa . If you wish to create your own catalogue, the required format is that each line should be 85 characters wide, with a wavelength in the first column, and the rest of the characters are not used by the code but are transferred to the output files. They can thus be used, as in the supplied catalogues, for line transition data. To use the default catalogues but exclude some lines, the --exclude-line option can be used.
Fit and subtract night sky emission lines before fitting nebular emission lines.
Write out upper limits for all lines searched for and not detected. The upper limit is calculated as the detection limit (default 3, set by −−detection-limit) multiplied by the uncertainty. In FITS output, this option is ignored - all upper limits are written out, and are indicated by negative flux values. If the FITS file is later anaysed with neat, these negative values are simply ignored.
−vg, −−velocity−guess [VALUE]
Initial guess for the velocity of the object [km/s]. Default: 0.
−vtol1, −−velocity−tolerance−1 [VALUE]
Variation allowed in velocity in first pass of the fitting. Default: 900km/s
−vtol2, −−velocity−tolerance−2 [VALUE]
Variation allowed in velocity in second pass of the fitting. Default: 60km/s
−wc, −−wavelength-column [INTEGER]
When reading FITS tables, this option can be used to specify in which table column the wavelength values are. For any other file type it will have no effect. Default: 1
−ws, −−wavelength−scaling [VALUE]
alfa checks the units of FITS file headers to set the wavelength scale, defaulting to assuming Angstroms if no keyword is present. If your input spectrum is not in Angstroms, use this option to set the value by which wavelengths should be multiplied to convert them to A. For example, −ws 10.0 would apply if your spectra have wavelengths in nm.
works in three stages. First, it estimates and subtracts the
continuum. Second, it estimates the resolution of the
spectra and the velocity of the object. And third, it fits
the emission lines. These stages work as follows:
alfa estimates the continuum using a percentile filter, taking the 25th percentile in a moving window 101 pixels wide. Currently these values are hard-coded, but will be user-configurable in a future release. Regions such as the Balmer and Paschen jumps may be poorly fitted by this method if the spectral resolution is low and the continuum gradient is changing fast. Broad stellar emission lines and telluric absorption features may also not be well fitted by this method. Inspection of the fitted continuum is recommended.
Estimation of the resolution and velocity
If no relevant command line options are specified, alfa begins by assuming that the velocity of the object is zero, and that the spectrum is Nyquist-sampled. It then carries out a fit on a subset of strong lines, using the genetic algorithm described below, to obtain an overall estimate for the velocity and the resolution. If necessary, the initial guesses can be specified with the -vg and -rg options described above, and the parameter space for the fine tuning can be specified with -vtol1 and -rtol1.
Fitting of the emission lines
With the continuum subtracted and the resolution and velocity estimated, alfa divides the spectrum up into chunks 440 pixels wide, with 20 pixels at either end overlapping with adjacent chunks. Then the genetic algorithm fits all lines from the deep catalogue that fall within the central 400 pixels, with the overlap regions providing the full line profile for lines close to the edge of the chunk. The initial guess for the resolution and velocity are taken from the global estimate for the first chunk, and from the preceding chunk’s fine tuned value for all succeeding chunks.
With the parameters optimised in each chunk, uncertainties are estimated using the root mean square of the residuals in a 20 pixel window, exlucing the two largest residuals to mitigate against overestimated uncertainties in the neighbourhood of bad pixels or strong lines.
alfa can read either plain text files or FITS format files. For plain text, the file should contain a wavelength and a flux, with the wavelength in the same units as the line catalogues (the default catalogues have wavelengths in Angstroms). FITS files are read using the CFITSIO library, so any FITS-compliant file should be fine. However, a surprisingly large fraction of all FITS files do not comply with the standard, so in case of problems, trying using fitsverify to check your FITS file.
The FITS file can have one, two or three dimensions. If it has two, it is assumed to be in Row-Stacked Spectra (RSS) format, while if it has three, it is assumed to be a data cube with two axes representing spatial dimensions and the third representing the spectral dimension.
If you don’t want to fit the whole dataset, you can specify the range of pixels on each axis that you want alfa to read in by appending the filename with [startx:endx,starty:endy]. This functionality is part of the CFITSIO library, and the format is described at https://heasarc.gsfc.nasa.gov/docs/software/fitsio/c/c_user/node97.html. alfa itself does not read in the coordinates of the section, and so the output file numbering starts from 1 on each axis regardless of where the image section actually started. The next release of alfa will have improved support for image sections.
alfa can produce output in plain text, csv, latex or FITS format. FITS is the default and recommended format; in future releases, output formats other than FITS will be deprecated and eventually removed.
plain text, csv or latex output, alfa will produce
two files, a fit file and a line list file. When producing
FITS format, a single file is created, with three
extensions, for the fit, the linelist, and a third extension
containing the Hbeta flux, number of lines detected, the
radial velocity and average resolution over the spectrum.
Output filenames are based on the input filename, with the
extensions noted below.
The fit file (_fit.txt, _fit.csv, _fit.tex) or extension (.fits):
The fit file
contains the best fitting synthesised spectrum. It contains
seven columns, representing the wavelength, the input
spectrum, the fitted spectrum, the original after continuum
subtraction, the estimated continuum, the fluxes of sky
lines, and the residuals. Thus, to see the fitted spectrum,
you need to plot columns 1 and 3 of this file. In gnuplot,
one can compare the input and fitted spectra using this
plot ’filename_fit’ w l, ’filename_fit’ using 1:3 w l
The lines file (_lines.txt,
_lines.csv, _lines.tex) or extension
This file contains four columns with parameters of the fitted lines - the observed wavelength, the rest wavelength, the flux, and the uncertainty estimated from the residuals. This file can be read directly by neat, which determines abundances for photoionised nebulae. If latex format is requested, the file additionally contains atomic data details not currently available in the other formats.
For RSS files and data cubes, alfa currently produces output for each pixel. Thus, for a large data cube you may end up with tens of thousands of files in the output directory. A routine to combine these outputs into image maps will be provided in a future release of alfa.
alfa’s default parameters are supposed to work in most cases, but sometimes you might find that it does not converge on the correct wavelength solution. It searches initially for velocities in the range +/-900km/s, which is very large for Galactic objects. So, running the code with --resolution-tolerance-1 100. or so may improve your results.
The genetic parameters (population size, number of generations, pressure) are likely to be suitable for most cases. There is no algorithm yet known for optimising these parameters in a genetic algorithm, so changing them requires trial and error. In spectra of regions with lots of emission lines, such as 4000-4500 Angstrom, increasing the number of generations can result in a better fit.
If reporting a bug, please state which version of alfa you were using, and include input and any output files produced if possible.