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These routines are contributions from research projects, they are not part of the ULySS package. These programs are not necessarily as extensively documented nor as well tested as the main package routines. They are provided with the hope they can be helpful.
Feed-back and submission of other routines are welcome.
| AUX_ALONG | Derive age/metallicity profiles for long-slit spectra |
| AUX_PLONG | Plot age/metallicity profiles for long-slit spectra |
| AUX_PSFH | Plot the SFH resulting from n-SSPs fit |
| AUX_READ_GALAXEV | Read a grid of GalaxEV models |
| AUX_READ_PEGASE | Read a grid of Pegase.HR models |
| AUX_READ_VAZMILES | Read a grid of Vazdekis models |
| AUX_SFH | Determine a star formation history |
NAME: AUX_ALONG PURPOSE: Derive age/metallicity profiles for long-slit spectra USAGE: aux_along, <obs>, <cmp>, <target_sn>, <file_out>, /PLOT, MD=md, KMOMENT=kmoment, CENTER=center DESCRIPTION: <obs> shall be a spect structure containing the long-slit spectrum. The program search the peak of light (center of the galaxy), and analyse the data successively from each side of the peak. The data are binned together to reach <target_sn>, but if the radial range assembled in one bin reach rmax/rmin=1.4 the target_sn is reduced. The profile is stopped when it is not possible to get a bin with sn>5. The output of this program is a series of FITS and res files, each of them corresponding to a single point of the profile. The file names are made by attaching 'r'<rad> to the prefix <file_out>, where <rad> is the value of the radius (positive or negative). ARGUMENTS: <spectrum> - input 2d spectrum structure (definined with ULY_SPECT_ALLOC) <cmp> - input Array of models' components, see ULY_FIT. Prior calls to ULY_STAR, ULY_TGM, ULY_SSP and/or ULY_LINE can define this array and set the guesses and constraints on the free parameters. MODEL_FILE can be given instead. <target_sn>- input Targeted S/N ratio; data are binned together to reach this value <file_out> - input, string output file name, to which suffix with the readious and '.res'/'.fits' are attached KEYWORDS: /PLOT Plot ulyss fit MD Degree of multiplicative polynomial, to be passed to ulyss (see ulyss.pro documentation) KMOMENT Number of terms in LOSVD, default 2 - velocity, velocity dispersion CENTER Index of the center line. By default it is automatically determined as the peak of light. HISTORY: MK: 2009/09 Creation PhP: 2010/05/25 Do the fit in 2 steps (first clean, after global minimization) Dismiss the bad fits (as much as I could) PhP: 2010/06/23 Make the program more general, to be usable for any longslit spectra MK: 2012/10/24 Documentation
(See aux_along.pro)
NAME: AUX_PLONG PURPOSE: Plot age/metallicity profiles for long-slit spectra USAGE: aux_plong, <nm>, PS=ps, /NOLOSVD, /NOPOP, CHI2=chi2, HOR_AGE=hor_age, HOR_MET=hor_met, VER=ver, /NOYTIT, /NYLAB, /LOGF, XTIT=xtit, CODK=codk, IRAD=irad, GALNAME=galname, XRANGE=xrange, CZRANGE=czrange, SIGRANGE=sigrange, AGERANGE=agerange, METRANGE=metrange DESCRIPTION: Plot the kin+SSP profile generated with the program AUX_ALONG Each point is a separate '.res' file named as: <nm>'_r'<rad>'.res' where <nm> is the generic name of the analysed frame, and <rad> is the position along the slit, in arcsec. ARGUMENTS: <nm> - input The prefix denoting the name (path+name) of the analysed frame; indentical to <file_out> in AUX_ALONG KEYWORDS: PS Save the plot in a postscript file named <ps> /NOLOSVD Do not plot the kinematics /NOPOP Do not plot the age/metallicity profiles /CHI2 Plot the chi2 values HOR_AGE [Gyr] Overplot age = [<real1>,<real2>]. For example the mean age at 1 arcsec and 1 effective radius HOR_MET [dex] Same as hor_age but for metallicity VER [dimensionless] Overplot as a vertical line the effective radius of the galaxy, real /NOYTIT Do not plot the title of the y-axes /NYLAB Do not plot the labels of the y-axes /LOGF Plot the flux in log XTIT x-axis title, string CODK [dimensionless] Coding of the symbols for each individual profile. Useful if few data sets are overplotted 0 : red/blue 1 : magenta/cyan 2 : 'black' 3 : continuous line IRAD GALNAME Name of the galaxy, to be overplotted in the right upper corner, string XRANGE default = [0, abs(max(<rad>))] array with the x-axis plotting range CZRANGE [km/s] Plotting range for cz SIGRANGE [km/s] Velocity dispersion range AGERANGE [Gyr] Age range METRANGE [dex] metallicity range HISTORY: MK: 2009/09 Creation, used for 2009MNRAS.396.2133K PhP: 2010/05/26 Modifications for 2011MNRAS.417.1643K MK: 2012/10/26 Documentation
(See aux_plong.pro)
NAME: AUX_PSFH PURPOSE: Plot the SFH resulting from n-SSPs fit USAGE: plot_sfr, <filename>, PS=ps, \OVER, TIMESHIFT=timeshift, MULTCNST=multcnst, \NORMAL, FILL=fill, XTITLE=xtitle, YTITLE=ytitle, YRANGE=yrange, OVER=over, _EXTRA=extra INPUTS: <filename> Name of a file containing results from multi-SSP fit with ULYSS, should end on ".res". string KEYWORDS: \OVER Overplot SFH TIMESHIFT [Gyr] shift the age of the components by a constant NORMAL Normilize the total mass to 1. It can be used together with MULTFRAC. In this case the total mass is first normilized to 1 and after multiplied by MULTCNST To get the total mass in Solar masses, multiply the component wieght by a constant. For example, in the case of standard input ulyss models and SDSS data, MULTCNST = 0.3127e7*D^2, where D^2 is the distance in Mpc (see http://ulyss.univ-lyon1.fr/models.html) FILL color of the area under the SFH curve XTIT x-axis title YTIT y-axis title YRANGE y-axis range _EXTRA any keywords accepted by IDL PLOT procedure OPTIONAL OUTPUTS: PS name of the output postscript file. Note that '.eps' will be authomatically added RESTRICTIONS: If a component without free parameters is used (for example a stellar spectrum) the program will fail because it looks for the parameters names to indentify the number of SSPs used for the fit PROCEDURE: EXAMPLE: aux_sfh, uly_root+'/data/VazMiles_z-0.40t07.94.fits', [uly_ssp(AL=[10,1000], AG=300.),uly_ssp(AL=[1000,13000])], 'test' loadct, 39 aux_psfh, 'test.res', color=40, thick=5, fill=220 HISTORY: 200X/XX/XX: MK, creation 2012/10/29: MK, documentation
(See aux_psfh.pro)
NAME: AUX_READ_GALAXEV RESTRICTIONS: This routine is not approved part of the ULySS package. It is not tested and was designed for a particular purpose. PURPOSE: Read a grid of GalaxEV models USAGE: grid = aux_read_galaxev( model_dir, $ WAVERANGE=waverange, VELSCALE=velscale, $ AGERANGE=agerange, METALRANGE=metalrange, $ MGFE=mgfe, QUIET=quiet ) ARGUMENTS: model_dir: string, directory where the SSP .txt files are located To read models with 2 Mg/Fe enhancements, give a string array with the two directories. KEYWORDS: WAVERANGE: Two element array giving the limits of the range to read, in Angstrom. For example WAVERANGE=[4000d,4786d]. By default the whole data range is read. VELSCALE: Size of the pixels in km/s. For example VELSCALE=30. If VELSCALE is not given, the models are not rebinned, ie. they are as stored in the disk file (in linear or log scale). AGERANGE/METALRANGE: Extracted region of the grid. Ages in log(Myr) and metallicities in dex. By default the whole data range is read. For example AGERANGE=alog([100,15000]),METALRANGE=[-1.4,+0.7] MGFE: Mg/Fe ratio. A value to be added in the header QUIET: Verbosity control RETURN: A structure containing the readed models with the associeted WCS (see also ULY_SSP_ALLOC) DESCRIPTION: This routine can be used to generate a new grid of models by reading the txt files produced by the program GalaxEv/galaxpl. It is useful when, for example, a new library, or a new version becomes available. The grid read by AUX_READ_GALAXEV can be saved to a file and afterward used to define a component with ULY_SSP. The set of GalaxEv grids of models provided with ULySS in the directory 'models/' were generated by this program. EXAMPLE: To read the latest version of GalaxEv/Miles and save it grid = aux_read_galaxev(uly_root+'/models/galaxev/bc2003_hrs_miles_0p1_ssp') uly_ssp_write, grid, uly_root+'/models/test.fits' TESTS: test_models, uly_root+'/models/test.fits' sp = uly_spect_read(uly_root+'/data/VazMiles_z-0.40t07.94.fits') ulyss, sp, uly_ssp(model=uly_root+'/models/test.fits'), /plot HISTORY: Mina Koelva 2011/11/11, modified version of aux_read_pegase.pro
(See aux_read_galaxev.pro)
NAME: AUX_READ_PEGASE RESTRICTIONS: This routine is not approved part of the ULySS package. It is not tested and was designed for a particular purpose. PURPOSE: Read a grid of Pegase.HR models USAGE: grid = aux_read_pegase( model_dir, $ WAVERANGE=waverange, VELSCALE=velscale, $ AGERANGE=agerange, METALRANGE=metalrange, $ MGFE=mgfe, QUIET=quiet ) ARGUMENTS: model_dir: string, directory where the SSP .FITS files are located To read models with 2 Mg/Fe enhancements, give a string array with the two directories. KEYWORDS: WAVERANGE: Two element array giving the limits of the range to read, in Angstrom. For example WAVERANGE=[4000d,4786d]. By default the whole data range is read. VELSCALE: Size of the pixels in km/s. For example VELSCALE=30. If VELSCALE is not given, the models are not rebinned, ie. they are as stored in the disk file (in linear or log scale). AGERANGE/METALRANGE: Extracted region of the grid. Ages in log(Myr) and metallicities in dex. By default the whole data range is read. For example AGERANGE=alog([100,15000]),METALRANGE=[-1.4,+0.7] MGFE: Mg/Fe ratio. A value to be added in the header QUIET: Verbosity control RETURN: A structure containing the readed models with the associeted WCS (see also ULY_SSP_ALLOC) DESCRIPTION: This routine can be used to generate a new grid of models by reading the FITS files produced by the program PEGASE_HR. It is useful when, for example, a new library, or a new version becomes available. The grid read by AUX_READ_PEGASE can be saved to a file and afterward used to define a component with ULY_SSP. The set of PEGASE_HR grids of models provided with ULySS in the directory 'models/' were generated by this program. EXAMPLE: To read the latest version of PHR/Elodie and save it grid = aux_read_pegase(uly_root+'/models/PEG_/e32_Salp_SB') uly_ssp_write, grid, uly_root+'/models/PHR_E32_test.fits' TEST: test_models, uly_root+'/models/PHR_E32_test.fits' sp = uly_root+'/data/VazMiles_z-0.40t07.94.fits' ulyss, sp, uly_ssp(model=uly_root+'/models/PHR_E32_test.fits') test_models, uly_root+'/models/PHR_E32_test.fits' HISTORY: Martin France, 2006, created Mina Koleva, 2007/10/18, debugged, upgraded
(See aux_read_pegase.pro)
NAME: AUX_READ_VAZMILES PURPOSE: Read a grid of Vazdekis models USAGE: grid = aux_read_vazmiles (model_dir, $ WAVERANGE=waverange, VELSCALE=velscale, $ AGERANGE=agerange, METALRANGE=metalrange, $ QUIET=quiet) ARGUMENTS: model_dir: string, directory where the SSP .FITS files are located To read models with 2 Mg/Fe enhancements, give a string array with the two directories. KEYWORDS: WAVERANGE: Two element array giving the limits of the range to read, in Angstrom. For example WAVERANGE=[4000d,4786d]. By default is [3000,10000] VELSCALE: Size of the pixels in km/s. For example VELSCALE=30. If VELSCALE is not given, the models are not rebinned, ie. they are as stored in the disk file (in linear or log scale). AGERANGE/METALRANGE: Extracted region of the grid. Ages in Myr and metallicities in dex. By default agerange=[0, 23000]Myr, metalrange = [-5.0, +3.0]dex. For example AGERANGE=[100,1500],METALRANGE=[-1.4,+0.2] QUIET: Verbosity control RETURN: A structure containing the readed models with the associeted WCS (see also ULY_SSP_ALLOC) DESCRIPTION: This routine can be used to generate a new grid of models by reading a series of FITS files containing the Vazdekis models with the Miles or CaII libraries. It is an analogue to AUX_READ_PEGASE. See also ULY_SSP_READ. EXAMPLE: Read and save a grid of Vaz/Miles to a single fits file grid = aux_read_vazmiles(uly_root+'/models/Vaz_/Miles') uly_ssp_write, grid, uly_root+'/models/Vaz_Miles.fits' Read and write the CaT library grid = aux_read_vazmiles(uly_root+'/models/Vaz_/caii') uly_ssp_write, grid, uly_root+'/models/Vaz_CaT.fits' LIMITATIONS: We hardcoded number of metallicity bins to 6 and number of age bins to 100. The program is working fine if the real numbers are equal or less than this but otherwise the user have to change. The same is true for the wave-, age-, metallicity- ranges.
(See aux_read_vazmiles.pro)
NAME: AUX_SFH RESTRICTIONS: This routine is not approved part of the ULySS package. It is not tested and was designed for a particular purpose. (Comments from PhP 2012/11/15) The determined SFHs are highly unstable and sensitive to degeneracies and the need for interations with various decompositions adds to the instability. The user can himself decide if it is reasonable to use this approach. PURPOSE: Determine a star formation history USAGE: aux_sfh, <nami>, <model>, <namo>, /CLEAN, DETECT_THRESHOLD=detect, STATUS=status, _EXTRA=_extra DESCRIPTION: The spectrum <nami> is decomposed in a series of bursts described in <model>. If this decomposition is considered as inacceptable, the model is modified (e. g. consecutive bursts are merged), and the procedure is iteratively called (re-entrant call). ARGUMENTS: model - model component nami - input name namo - output name KEYWORDS: CLEAN - perform the fit twice - clean and then fit _EXTRA - keywords to be passed to ulyss HISTORY: this program was send by Mina (2010/05/26) It is analysing some spectra to find the SFH in 3 bursts PhP: I modified this program to read the files from GMOS/Spolaor Do the fit in two passes (clean and then global minimisation) Rewrite the program to work for any number and characteristics of bursts in the SFH decomposition (PhP 2010/05/30 and 31st). Generelize the program to work for arbirary components (not only ssps). For the moment the component should consiste of ssps+other definitions (MK 2012/05/26)
(See aux_sfh.pro)
uly_html_help.| Contact: ulyss at obs.univ-lyon1.fr |
Last modified: Mon Oct 26 10:55:15 2015. |