This is: http://sail.zpf.fer.hr/cres/, last update 12. June 2006.
A tool for resolving of spectra of components of multiple stellar systems.Saša Ilijić, Dept of Applied Physics, FER, Univ. of Zagreb, Croatia
Contents: Overview, Obtaining and installing, Example run using artificial data, TIFR case: normalisation procedure, Example run using real data: HD 23642, References, Address
For a large class of geometrically unresolved binary stars and higher multiplicity stellar systems one may assume that the observed spectra are composed of time independent spectra of component stars that add together with time dependent orbital RV-shifts, and possibly with time dependent flux-ratii. The observed spectra of such systems usually contain complicated blends of spectral features of component stars and are difficult to analyse. The spectral separation algorithm, introduced by [BG91] and later reformulated by [SS94], see also [H95], takes a time series of such spectra, together with RVs and relative flux contributions of components in each observed spectrum, and attempts to resolve the spectra of component stars.
The code CRES implements the spectral separation algorithm in a very general and flexible, but computationally demanding way. The least squares fit to the data is obtained with the singular value decomposition technique in the wavelength domain [SS94,I03,I04]. What makes CRES unique compared to other tools for spectral separation, eg. [FDBinary,KOREL], is that
Theoretically CRES can handle any amount of input data and it can try to resolve any number of component spectra. However, the required CPU-time is likely to set limits to the size of the data set that can be handled.
NOTE: The so called spectral disentangling technique goes one step further by optimising the RVs. CRES does not do that. It is intended for critical work in spectral separation once the RVs have been determined.
I make the code CRES available under the terms of the GPL. If publishing with CRES please refer to [I04]
Ilijic S, 2004, Thoughts about disentangling in wavelength and in Fourier space, ASP Conf Ser 318, 107-10
(preprint: ps.gz, pdf) in your publication. Basically CRES consists of two files:
Please observe comments in these two files.
In several steps I will show how to reproduce the example of Figure 1 [PDF] in [I04].
These are ordinary "data-files" with three numbers per line: wavelength, amplitude and estimated error. The files may cover a wider wavelength range than the one that is going to be used. The files in this example are: c1.obs, c2.obs, c3.obs, c4.obs, c5.obs, c6.obs, c7.obs, c8.obs and c9.obs. In this example sampling in wavelength is regular, but note that it does not have to be that way.
The spectral range, radial velocities (RVs) and light-factors (LFs: fractional contributions component continua to the continuum in the composite spectrum) must be supplied for each component and for observed spectrum. This information is collected into one file. In this example this cresprep.in, see comments inside for description of the syntax.
The file cresprep.in created in Step 2 should be processed through the cresprep.pl script to prepare the input file for cres.eqs CRES. On my computer it went like this:
$ ./cresprep.pl < cresprep.in > cres.eqs
each line in the file cres.eqs, called "equations-file", provides all information needed to assemble one equation of the fit. The last line of the "equations-file" (if created with cresprep.pl script) specifies the total number of equations. This is easily displayed with:
$ tail -1 cres.eqs
# nr of data pts (eqns) in this file: 900
You may simply launch CRES and feed the input from the keyboard when asked (your screen would look like this screen-shot), but it is much safer and easier to prepare a simple input file like cres.in in this example. It is also wise to direct the screen output of CRES into a file for later reference, here this is cres.out. The command line in this example is:
$ ./cres < cres.in > cres.out
The calculation will, however, take some time. Running the job in the background is recommended. Note that cres.out is equivalent to the screen shot shown above, ie. it repeats all input parameters given in cres.in.
The number of input files depends on the way CRES is used. Their names are generated by appending suffices to the name of the "equations file". In this example CRES creates the files:
The format of model spectra files is: wavelength, amplitude, estimated error. CRES automatically distributes the requested number of points (free parameters) equidistantly in the logarithm of the wavelength to cover the spectral range in which the component spectrum can be re-constructed from the data set.
The format of the residuals file is: obswavelength, obsamplitude, obserror, observedminuscalcamp, hashcharacter, code. To extract residuals corresponding to one observed spectrum, say one with the "C3" you can use:
$ grep C3 cres.eqs.res.s01 > c3.res
In this example the lowest "singular value" is of the order of the machine precision, and is therefore considered singular, while all other can be considered regular. This is expected whenever the light-factors (relative contributions of component continua to observed continuum) of the component stars do not change with the observed spectra. The consequence of this is that the output component spectra in cres.eqs.m01.s01 and cres.eqs.m02.s01 are not correctly normalised. See next section.
In time-independent flux-ratio (TIFR) case the light factors (LFs) of the component stars do not change among the observed spectra. The component spectra calculated by CRES are not as such correctly normalised. The normalisation procedure to be used with CRES, applicable for N component spectra whose modeled by different numbers of free parameters (wavelength points), is coming soon.
For the special, but most useful, case of resolving two component spectra that are modeled by the same number of free parameters (wavelength points) the normalisation procedure [IHPF04] formulated for the Fourier-based disentangling code [FDBinary] can be safely used without changes.
In the paper [U04], dealing with the distance to the Pleiades open cluster, Munari and co-workers analysed the binary HD 23642. They obtained five spectrograms at Observatorie de Haute Provence, France, with the ELODIE spectrograph in Feb. 2004. In the Table 1 of the paper they give the component RVs they measured, and the reduced spectrograms (deblazed flux, orders not merged) are available at the dedicated web page. I use these data to provide an example of using CRES to resolve the spectra of component stars.
Not going to undertake merging of orders, I can separate only the central regions of individual orders. The spectrograms are first filtered through a procedure that removes the data points that are likely to be outliers. Another automatical procedure performs continuum normalisation of the spectra in the selected spectral range. Both procedures are very simple, and could be significantly improved for more critical work.
The five files containing continuum normalised data in the wavelength range 5160A-5180A, extracted from the order #39 with the automatical procedures, are Feb03_218689.obs, Feb03_228489.obs, Feb04_000949.obs, Feb07_179842.obs and Feb10_180764.obs. The RVs corresponding to the spectra, originating from [U04 Table 1] are put into the cresprep.in. Note that all light factors are set to the value 0.5, which is in accord with the assumed TIFR [IHPF04]. CRES is run like this:
$ ./cresprep.pl < cresprep.in > cres.eqs
$ ./cres < cres.in > cres.out
Since we are in the TIFR case we use the output files that correspond to the first singular value discarded. These are the model component spectra cres.eqs.m01.s01, cres.eqs.m02.s01, and the residuals cres.eqs.res.s01.
The input data are shown in black lines with the error bars indicated by the dots one sigma above and below, shift in the relative amplitude is applied among the spectra for clarity. The component spectra for the brighter and the fainter component are shown in green and blue respectively, estimated errors shown with dots. Component spectra are normalised using the procedure described in [IHPF04] with the values b=0.035 for the average line-blocking in the input spectra and L=4 for the component flux-ratio (taken from [U04 Table 2]). The residuals of the fit are shown against the data in red colour. This figure is available in higher resolution in PDF format: 3951605180.pdf
Procedure equivalent to the one described above was carried out in several other spectral regions (echelle orders):
Please note that the results shown are intended only for presentation of the capabilities of the code, and are not part of other research.
|BG91||Bagnuolo W G, Gies D R, 1991, ApJ 376, 266 [ads]|
|SS94||Simon K P, Sturm E, 1994, AA 281, 286 [ads]|
|H95||Hadrava P, 1995, AAS 114, 393 [ads]|
|IHP01a||Ilijic S, Hensberge H, Pavlovski K, 2001, Springer LNP 573, 269 [ads]|
|IHP01b||Ilijic S, Hensberge H, Pavlovski K, 2001, Fizika B 10, 357 [Fizika B]|
|I03||Ilijic S, 2003, M.Sc. thesis [pdf]|
|I04||Ilijic S, 2004, ASP Conf Ser 318, 107 [preprint: ps.gz, pdf]|
|IHPF04||Ilijic S, Hensberge H, Pavlovski K, Freyhammer L M, 2004, ASP Conf Ser 318, 111 [poster: pdf, preprint: ps.gz, pdf]|
|U04||Munari U, Dallaporta S, Siviero A, Soubiran C, Fiorucci M, Girard P, 2004, A&A 418L, 31 [ads, arXiv]|