It is now possible to give and use as constraints the equivalent widths of lines outside the observed spectral range (useful if you get the information from somewhere else).ħ. Added the possibility, when fitting a whole data cube, to use a mask indicating where the fit has to be performed.
Equivalent widths are now measurable at fixed, custom-defined passbands,as well ĥ. It is now possible to choose the age of the oldest SSP in a consistent way with the adopted cosmology Ĥ. The spectral normalization wavelength is now customizable ģ.
Most of the default input file are now more consistently “customizable”, and in case they will have to be located in the directory where sinopsis is run (cosmology, continuum band definition, stellar population parameters definition) Ģ. Big thanks to Dani Díaz for implementing an installation script that should make things much easier and automatic.Īmong the new features (with respect to version 1.6.4, the latest here described):ġ. An example of the set up file ( config.sin) is also given, together with examples of input catalogs in various format. A python script will very soon be available to visualize the results of the fit. The source code, together with all the needed models and files, can be instead downloaded from GitHub upon request (drop me an email!).
#Sinopsis a muse download#
To have a quick look on SINOPSIS’ installation, usage, options, and possibilities, you can download its (incomplete, for the moment) USER MANUAL. As long as you want to use it to reproduce a set of optical spectra (or even only 1), you should be able to do it right away, after downloading and compiling it. Nevertheless, some of the options are still on a test phase (e.g. SINOPSIS is currently (July, 2018) a very well tested tool, as it was used to fit and interpret the spectra of more than 10 4 galaxies, including integral field data. Here you can find a couple of examples of fits and Star Formation History reconstructions.
#Sinopsis a muse code#
The basis of this model rely on the spectral fitting code that was used to reproduce and analyze WINGS optical spectra. 2014, and we are currently working on it to make it even more robust and reliable. This method is described in detail in Fritz et al. the “selective extinction” hypothesis: younger stars tend to be more affected by dust extinction with respect to the more evolved ones).Īnother advantage of SINOPSIS is that it uses a very robust method to calculate the equivalent width of spectral lines, even in low S/N spectra, that are used as constraints to derive the star formation history of a galaxy. Furthermore, it adopts a treatment of extinction that can be, in principle, fully dependent on the stellar age (i.e. SINOPSIS is currently one of the few spectral fitting codes available in the literature which does not assume any pre-determined star formation history and that uses no pre-computed libraries. The code has evolved since then, becoming more powerful, versatile and fast, but the idea is pretty much the same. The roots of the code can be found the paper by Poggianti, Bressan & Franceschini, 2001. It combines the theoretical spectra of Simple Stellar Population models (SSP) with templates of the near, mid, and far infrared (NIR, MIR, FIR) emission (DISCLAMER: the FIR option is still under developing). SINOPSIS is a spectrophotometric fitting code which aims at reproducing the combined spectral and broad-band photometric data of galaxies.
0 kommentar(er)
