A Tool for Astrophysical Data Analysis user manual
Contents
1. e gt 5 6 A A o w g e e s parameter 1 Figure 2 3 Examples of allowed top row and not allowed bottom row configurations for a user supplied 2 dimensional grid of stellar parameters F TA DA Tool for Astrophysical Data Analysis 5 amm ev Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fiter Do you want to use evolutionary models or an arbitrary set of parameters C Evolutionary Models Please provide Teff K Log g cgs Radius Rsun teff_logg_rbt 5 rows E Select ascii file 19 L TADAS example input files 4 Search exam Organize folder Name Date modified Type 17 big_logt_logl tt 7 2011 4 48 PM Text Document catalog_table_NEW dat 6 46PM DATFile mass_agebt 3 17 35 PM Text Document teff logg rbd 3 15 20 0 01PM Text Document Type Text Document Size 74 bytes Date modified 3 15 2011 10 01 PM File name E Figure 2 4 Importing a set of values of Tig gravity and stellar radius the 3rd column of the ASCII file can be arbitrary for example 1 Re for every model point In the first panel clicking on the Submit button will lock in the input parameters TA DA organizes the set of stellar parameters perform any interpolation if needed c2. 13 527 0573574197 05 28 12 7 13 240 0 005 12 297 Advanced selection Select the first lines on the current sorted table Select the first lines on the current page User defined IDL logical sting fen wv le 4 example gt 15 and col4 sqit col5 le 1 Figure 2 7 Example of ASCII table imported to the TADA e A right click is for the closest model point to the clicked point a popup windows is created showing the parameters associated to that point e g mass age log Teg log L stellar radius log g as well as the value of the quantities plotted in the two axes e g color and magnitude Clearly whereas the right click will in general always work results of synthetic photometry always appear in the plot the left click will work only if a table with the observed photometry is attached the two quantities plotted are specified and at least one star is selected from the table panel Adding labels to the plot By default the plot window shows a label located in the top left corner reporting the name of the used evolutionary models and synthetic spectra It is possible to customize the label remove it displace it or change the information reported This can be done by editing the file tada_data tadaplot_additional_instructions dat within the TA DA installation directory where the actual IDL code lines which produce the label are declared Further explanations on how to do this as well a
3. B WFC3UVIS_F645N WFI_V ACSVVFC F475VV NIRCAM_F070W STROMGREN OLD U WFC3UVIS_F656N VVFPC2 F170VV ACSWFC_F502N NIRCAM FO9OVV STROMGREN U WFC3UVIS_F657N VVFPC2 F255VV ACSWFC_F550M NIRCAM F115VV STROMGREN V WFC3UVIS_F658N WFPC2_F300W ACSVVFC F555VV NIRCAM_F140M STROMGREN Y WFC3UVIS_F665N WFPC2_F336W ACSVVFC F606VV NIRCAM F150VV TYCHO B WFC3UVIS_F673N VVFPC2 F380VV ACSWFC_F625W NIRCAM F150VV2 TYCHO_V WFC3UVIS_F680N VVFPC2 F439VV ACSWFC_F658N NIRCAM_F162M WFC3IR_F098M WFC3UVIS_F689M WFPC2_F450W ACSWFC_F660N NIRCAM_F164N WFC3IR_F105W WFC3UVIS_F763M WFPC2_F467M ACSWFC_F775W NIRCAM_F182M WFC3IR_F110W WFC3UVIS_F775W WFPC2_F502N ACSVVFC F814VV NIRCAM F187N WFC3IR_F125W WFC3UVIS_FSI4W WFPC2_F547M ACSVVFC F850LP NIRCAM_F200W WFC3IR_F126N VVFC3UV1S F845M VVFPC2 F555VV BESSELL B NIRCAM F210M WFC3IR_F127M WFC3UVIS_F850LP VVFPC2 F569VV BESSELL BVV NIRCAM F212N WFC3IR_F128N WFC3UVIS_F953N WFPC2_F606W BESSELL I NIRCAM F225N WFC3IR F130N WFC3UVIS_FQ232N VVFPC2 F631N BESSELL_R NIRCAM F250M WFC3IR_F132N WFC3UVIS_FQ243N WFPC2_F656N BESSELL_U NIRCAM F277VV VVFC31R F139M WFC3UVIS_FQ378N WFPC2_F673N BESSELL_V NIRCAM F300M WFC3IR_F140W WFC3UVIS_FQ387N WFPC2_F675W CFHT_H NIRCAM F322VV2 WFC3IR_F153M WFC3UVIS_FQ422M WFPC2_F702W CFHT I NIRCAM F323N VVFC31R F160VV VVFC3UV1S FQ436N VVFPC2 F785LP CFHT_J NIRCAM F335M WFC3IR_F164N WFC3UVIS_FQ437N VVFPC2 F791VV CFHT_KS NIRCAM F356VV WFC3IR_F167N WFC3UVIS_FQ49
4. Settle grid of Allard et al 2010 defined for 2000 K lt Tig lt 70 000 K 0 5 lt log g lt 5 5 1 lt M H lt 0 3 The NextGen grid of Hauschildt et al 1997 defined for 2500 K lt Tig lt 50 000 K 2 lt log g lt 5 5 1 5 lt M H lt 0 e The NextGen grid of Hauschildt et al 1997 complemented with the AMES MT grid of Allard et al 2001 for the low Teg defined for 2000 K lt Tog lt 50 000 K 34 logg 5 5 M H 0 The AMES Settle grid of Allard et al 2002 defined for 1100 K lt Tig 2300 K 4 5 lt log g lt 5 5 1 lt M H lt 0 One can add additional grids by placing them in a proper format in the same directory The grid of spectra must include a spectrum as a function of 3 parameters the first 2 must be Teg in Kelvin and logg in logarithm of cm s the third parameter is typically metallicity M H but can be any other arbitrary quantity The grids of spectra must be stored as a 5 column fits table where the columns are 1 wavelength in Angstrom 1 dimensional nlambda elements 2 Teff in Kelvin 1 dimensional nmodels elements 3 log g in log of cm s 1 dimensional nmodels elements 27 4 third parameter whatever units e g metalliticy in M H 1 dimensional nmodels elements 5 the actual spectra in erg s 7 cm A 1 2 dimensional nmodels x nlambda elements The fits tables must also include these additional keywords in their headers NAME Am
5. The user can then use these values to discern among solutions to be kept or rejected Although this applies to both the case of interpolation of parameters and SED fitting there is a significant conceptual difference between these two cases 19 e in the interpolation case number of free parameters number of fitted observed quanti ties if a star is located within the modeled grid an exact solution is always found x 0 Thus the fitter precisely distinguish between points inside or outside the grid flags sources accordingly and use the correct method to provide the best fit parameters Figure 10 schematizes the process for the two sub cases a and b for a 2 dimensional magnitude space in the actual SED fitting case number of free parameters number of fitted observed quantities an exact solution x 0 is generally never found Thus TA DA arbitrarily considers stars to be incompatible with the model grid when they lie at gt 30 from the edge of the grid In any case the results of the fitter include for every star two parameters that are useful to understand the goodness of the fit 1 exact is 1 if the observed star lies inside the parameter space covered by the model 0 otherwise see above distance in sigma reports the distance in units of the overall photometric error from the observed magnitude colors or fluxes of the star to the closest best fit point of the model g
6. al 2011 These are located as fits table files in the directory tada data isochrones The PISA Franec grids include a large number of isochrones for several metallicities mixing length parameter he lium abundance and deuterium abundance For this reason the original installation package of TA DA tada zip downloadable from the website includes only the most used models for solar metalliticy The rest of the grid can be downloaded if needed separately from the TA DA website To add new family of models one must put a properly formatted file containing them in this directory Specifically this must be a fits table must contain 4 columns in this order 1 mass in units of 2 logage in logarithm of years 25 3 log Ter in logarithm of K 4 log in Lo The header of the fits table must also include the following additional keywords e NAME the name of the family of models e g Siess 2000 oversh e SHORTNAM a shorter with no spaces name e g siessover M H the metallicity M H e g 0 0 float e MTYPE the type of models e g PMS not used by TA DA e coli mass content of the first column not actually used by TA DA so please do not change the order of the four 12 logage content of the second column e col3 logt content of the third column e co14 logl content of the fourth column Here we have an example of how to produce a valid format
7. fits table from IDL I will assume you have already 4 IDL variables named mass logage Logt logl as one dimensional arrays of floating point numbers containing this quantities 1111 fileout your path girardi_models fits FXHMAKE hdr EXTEND FXWRITE fileout hdr FXBHMAKE newhdr 1 FXBADDCOL c1 newhdr mass FXBADDCOL c2 newhdr logage FXBADDCOL c3 newhdr logt FXBADDCOL c4 newhdr 10g1 FXADDPAR nevhdr NAME Girardi et al 2000 FXADDPAR newhdr SHORTNAM girardi FXADDPAR nevhdr MTYPE postMS FXADDPAR nevhdr M H 0 0 FXADDPAR nevhdr col11 mass FXADDPAR nevhdr co12 l1ogage FXADDPAR nevhdr co13 logt FXADDPAR nevhdr co14 1ogl FXBCREATE unit fileout neuhdr FXBURITE unit mass c1 1 26 FXBWRITE unit logage c2 1 FXBWRITE unit logt c3 1 FXBWRITE unit logl c4 1 FXBFINISH unit 333333333939393939399339999399993939393933933393333393393939395 Important note the grid of evolutionary models must be already densely interpolated with a resolution in the parameter space not much worse than the precision you aim to achieve in fitting your data with TA DA and rectilinear in mass and log age see Figure 2 3 for what this means Synthetic spectra The current version of TA DA includes a number of grids of synthetic spectra used to perform synthetic photometry These are The BT
8. in the 2 parameters listed in the ASCII table i e a cartesian grid with arbitrary spacing between lines and columns no holes and not necessarily complete at the edges In Figure 2 3 some examples of allowed and not allowed configurations are shown for clarity The distinction between a 1 or 2 dimensional inputs is relevant only when one runs the fitter within TA DA and is irrelevant for the computation of the synthetic photometry In particular if the parameters represent a 2D grid the fitter will interpolate over the grid until the solution is found The options a and c are very similar since they both load the entire parameter space covered by the models Nevertheless there are two main differences between them First the option all isochrones has a finer sampling in masses whereas all tracks has a finer sampling in ages Therefore if the ultimate goal of the user is a precise estimate of stellar masses selecting all isochrones is more appropriate and viceversa Second when plotting the result of synthetic photometry TA DA will plot individual isochrones or tracks according to the choice done here 2 1 2 No evolutionary models defining only Ter logg R TA DA also allows to specify a more general set of stellar parameters which is independent on stellar evolutionary models This method is activated selecting Arbitrary option on the upper right part of the first panel In this case see Figur
9. newhdr NAME The name of my grid FXADDPAR nevhdr MODTYPE Star FXADDPAR nevhdr PARN 3 FXADDPAR nevhdr WAVN size lambda 1 FXADDPAR nevhdr WAVUNIT Angstrom FXADDPAR nevhdr PARNAME1 T FXADDPAR nevhdr PARNAML1 Temperature FXADDPAR nevhdr PARUNIT1 K FXADDPAR nevhdr PARLOG1 O 28 FXAD FXAD FXADI FXAD FXAD FXAD FXADI FXADI FXAD FXADI FXAD FXAD FXAD FXAD FXADI FXBC FXBW FXBV FXBW FXBW FXBV PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PAR nevhdr PA PA PA PA PA PA PA PA PA PA PA PA PA PA RMIN1 min teff RMAX1 max teff RNAME2 1ogg RNAML2 Surface gravity RUNIT2 1og cgs RLOG2 1 RMIN2 min logg RMAX2 max logg RNAME3 M H RNAML3 Metallicity RUNIT3 log ratio RLOG3 1 RMIN3 min metallicity RMAX3 max metallicity PAR newhdr MODN n_elements teff FXBFINISH unit REATE unit filename neuhdr RITE unit lambda c1 1 RITE unit teff c2 1 RITE unit logg c3 1 RITE unit metallicity c4 1 RITE unit spectra c5 1 Conte
10. 133280 0 035000 122980 0 0240000 AAA 222 m 000 19 2011 1140 VizeR 83753434 6355460 205350082 05380 11 9000 00240000 1107890 0032000 1030220 010210000 AAA 22 m 000 T 2011110 aer 83768101 56419790 0535043405382 13 5540 00410000 1122800 0105000100 11 6630 00 0300000 AAA 22 m 500 201 1110 Maier 83774076 56410680 105350577 05382 16 0520 0 0590000 14 0240 01450000 128220 010210000 AAA 22 m 000 201 1110 Maer 83769215 56438700 05350461 0538214 1310 010430000 125140 0105000100 11 3210 0002400100 AAA 22 m 000 19 2011 11 10 VizeR 83 807352 56527990 05351376 05391 10 8240 00210000 100270 0103000100 9 68200 0010210000 AAA 22 m 000 RF 2011110 VizeR 83803458 56521580 05351282 05331 12 8980 0102401000 113430 00320000 115040 01 0210000 AAA 222 m 00 201 1110 VizeR 83811982 56348680 05351487 0538 13 0170 0 023000 120130 0 330000 11 5090 00190000 ARA 222 m 000 RF 2011110 VizeR 83800438 56403720 05351210 05382 16 7680 00230000 153100 0 156000 155480 0 170000 022 on Occ 2011110 VizeR 83793437 6401750 105351042 053829 78800 0 023000 9 10300 0030000 83 78800 00190000 AAA 222 m 000 T 201 11 10 VizeR 83 782302 5465510 05350775 0538416 2050 010860000 1144330 0047000 134790 00230000 AAA 22 m 000 F 20110 aer 83 785998 5 6418090 05350863 05384 14 3230 010280000 1130560 0 0370000 1243360 00190000 AAA 22 m 000 TT 20ft 11 10 Maer 83 774113 5644130 105350578 05381 14 8320 00320000 133820 0103300100 123800 0010130000 AAA 22 m 000 T 201 11 10 Maer 83 780538 56447180 053
11. 2N VVFPC2 F814VV CFHT_Y NIRCAM_F360M WFC3UVIS_F200LP WFC3UVIS_FQ508N WFPC2_F850LP COUSINS I NIRCAM F405N WFC3UVIS_F218W WFC3UVIS_FQ575N WHITE_WHITE To add new filters it is sufficient to put a file containing its profile in the same directory This 23 24 must be a 2 column ASCII file with a name instrumentname_bandname dat The first column is the wavelength in Angstrom the second is the associated filter throughput The scaling units of the throughputs are absolutely irrelevant e g the peak could be 1 or not In case of broad band filters make sure that the profile you have includes also the other instrumental efficiencies e g the transparency of the optics and most importantly the detector efficiency as a function of wavelength Tf your filter has a VegaMag zeropoint which is the magnitude of Vega in that filter different than zero which is the case for some old photometric systems this value should be added in the file tada_data zeropoints dat following the format of the entries in the same file Evolutionary models The present version of TA DA includes already a number of evolutionary models namely e for evolved population e g globular clusters Marigo et al 2008 models e for pre main sequence populations Palla amp Stahler 1999 models Siess et al 2000 models Baraffe et al 1998 models D Antona amp Mazzitelli 1998 models PISA Franec models from Tognelli et
12. 50732 05394 14 0410 0 0280000 1124390 0 0300000 11 6270 0010230000 AAA 222 m 000 2011 11 10 Maer 83791187 56535950 105350988 05391 18 7930 00280000 153270 0 030000 155120 0 165000 WUC 002 on 000 Advanced selection Select theft Ines on the curent ted tabis Select the fist ines on the curent page User defined IDL logical sting E_JMAG le 0 025 example col gt 15 and col4 sat col5 le 1 Figure 2 8 Example of user data table attached to TA DA originally in format of VOTable TA DA Plot window m 8 E TA DA User data table m 8 catalog_table_NEW dat found 14 colum 0579451 Av 0 000000 Rv 3 10000 y Export postscript max Y 1523 selected ea ool F rz F r fona sort selection sot sr sr sot none al hot used rot ug e wit ferwe1 frotused 05 39 8626 0 027 992 F 002 05 35 8 822 0021 660 F 003 05 38 9280 0 036 260 F 0004 05 34 9425 0 016 Wodata VVFLV F 0005 05 35 9538 0 018 670 0006 05735 WFI_TI620 x 9 552 0 016 831 0007 05 34 9 596 0 018 nodata oog 05 34 9616 0 023 108 9 09 05 35 9 652 0 019 Wodata F oo 05 34 9 734 0021 45 05735 9 836 0 015 531 012 05 35 9913 0 010 odata 19 0013 05734 9 963 0 012 nodata V 0014 05734 10 001 0 017 nodata 0015 05 36 min Y 10 034 0 012 273 00706787 F oe 05 35 10 037 0 010 640
13. Cardelli reddening law is selected Synthetic photometry will be performed separately for each of these n Ay x n Ry values on every stellar parameter point provided in Panel 1 If the user wants to leave reddening as a free parameter to be fit to the observational data last panel of TA DA widget GUI see next sections it is mandatory to indicate at least 2 distinct values of Ay e g O and 1 in this field e Distance modulus a unique value for the distance modulus in magnitudes to be applied to the computed magnitudes or fluxes must be specified in this field e Photometric bands the user specifies multiple up to 16 photometric bands in which synthetic photometry has to be computed These can be selected through drop down menus separately for the instrument or photometric system and the filter The filter throughputs are stored as individual files in a TA DA installation subdirectory tada_data throughputs The convention for the filenames is instrument_filter dat and they contain a 2 column ascii indicating wavelength in A and throughput arbitrary relative units TA DA scans the content of this directory at start so additional photometric systems or bands can be added by simply placing the relative files describing the filters profile in the appropriate directory See the appendix for further details By clicking the submit button the synthetic photometry code is started according to the selected parameters a
14. F460M WFC3UVIS_F336W WFC3UVIS_FQ727N ACSHRC F330VV IRAC_I3 NIRCAM_F466N WFC3UVIS_F343N WFC3UVIS_FQ750N ACSHRC_F344N IRAC 14 NIRCAM F470N VVFC3UV1S F350LP WFC3UVIS_FQ889N ACSHRC F435VV ISAAC F1215 NIRCAM F480M WFC3UVIS_F373N WFC3UVIS_FQ906N ACSHRC F475VV ISAAC_F1710 SDSS G WFC3UVIS_F390M VVFC3UV1S FQ924N ACSHRC F502N ISAAC_F2090 SDSS_I WFC3UVIS_F390W WFC3UVIS_FQ937N ACSHRC F550M ISAAC_F3280 SDSS_R WFC3UVIS_F395N VVFL571 ACSHRC F555VV ISAAC FL BB SDSS_U WFC3UVIS_F410M WFI_753 ACSHRC F606VV JOHNSON_B SDSS_Z WFC3UVIS_F438W WFI_770 ACSHRC F625VV JOHNSON_U STISCCD 5OCCD WFC3UVIS_F467M VVFL851 ACSHRC F658N JOHNSON_V STISCCD_F28X50LP WFC3UVIS_F469N WFI_852 ACSHRC F660N LANDOLT B2 STISFUV_25MAMA WFC3UVIS_F475W WFL853 ACSHRC F775W LANDOLT_B3 STISFUV_F25LYA WFC3UVIS_F475X WFI 870 ACSHRC F814VV LANDOLT_U STISFUV F25QTZ VVFC3UV1S F487N VVFLB ACSHRC F850LP LANDOLT_V STISFUV_F25SRF2 WFC3UVIS_F502N VVFLB842 ACSHRC_F892N NICMOS_F110W STISNUV_25MAMA WFC3UVIS_F547M VVFLFLAT ACSSBC F115LP NICMOS_F160W STISNUV_F25CIII WFC3UVIS_F555W WFLHA ACSSBC F122M NICMOS F165M STISNUV F25CN182 WFC3UVIS_F600LP VVFLI ACSSBC F125LP NICMOS F187VV STISNUV_F25CN270 WFC3UVIS_F606W VVFL1879 ACSSBC F140LP NICMOS F190N STISNUV_F25MGII WFC3UVIS_F621M WFI_TI620 ACSSBC F150LP NICMOS_F205W STISNUV_F25QTZ WFC3UVIS_F625W VVFLU ACSSBC F165LP NICMOS F207M STISNUV F25SRF2 WFC3UVIS_F631N WFI_U841 ACSVVFC F435VV NICMOS F222M STROMGREN
15. TA DA A Tool for Astrophysical Data Analysis version 0 98 user manual Nicola Da Rio ndarioOrssd esa int August 8 2012 TA DA was developed thanks to funding from the NASA Award Number NNX07AT37G Chapter 1 Introduction 1 1 What is TA DA TA DA is a powerful integrated tool for the analysis of stellar photometric data aimed to significantly simplify the process of comparing stellar photometric data with theoretical models In the released version TA DA allows to easily and reliably operate on synthetic photome try creating theoretical spectral energy distributions SEDs The tool also supports analysis of photometry from different archives SED model fitting self consistent prediction of stellar parameters based on multi band photometry TA DA includes a comprehensive and updatable repository of throughputs of astronomical instruments and filters stellar and synthetic spectra and evolutionary models Photometric and spectroscopic data can easily be imported from the Virtual Observatory as well as from user s own tables and models Results are produced in tabular or graphic format readily usable for publication TA DA runs as an IDL widget application publicly available for download 1 2 TA DA functionalities We summarize here the main functionalities of TA DA 1 Computation synthetic photometry of complete grids of evolutionary models or part of them or any arbitrary set of stellar parameters Observed fluxes or mag
16. d by the spectra for the Teg of that point is neglected in the computation of the synthetic photometry If the option is activated magnitudes and colors of parameter points with a logg out of range are extrapolated from synthetic photometry within the covered logg range This extrapolation is useful when some model points correspond to logg values located just outside the grid An example of such scenario is when the spectra from the AMES grid of Allard et al 2000 defined for log g gt 3 5 is selected together with PMS evolutionary models which predict log g gt 3 2 for the youngest ages in the very low mass range Since in general the computed magnitudes and colors depend only weakly on log g extrapolating the results to a small extent outside of the grid still provides acceptable results The users should however be careful in selecting this option making sure they are aware of the parameter space covered by their stellar parameters and the grid of spectra 11 e Dust extinction extinction can be added directly to the synthetic spectra before the computation of the synthetic colors and magnitudes TA DA currently includes the Galac tic Cardelli 1989 extinction law as well as the the reddening curves for the Magellanic Clouds from Gordon et al 2003 LMC average LMC2 supershell SMC bar The user specifies one or more values of V band extinctions Ay and one or more values of the rel ative extinction parameter Ry only if the
17. ds to use for estimating the stellar parameters The available bands are those for which synthetic photometry was previously computed The user should keep in mind to select only bands for which the observed magnitudes or fluxes are provided and declated in the table window Clearly at least 2 bands must be selected Next the user can specify if the fit should be performed on the magnitudes in a n dimensional magnitude space or on the colors in a n 1 dimensional color space The latter option is useful 18 when the particular astrophysical problem the user is interested to solve requires the assessment of the stellar parameters in a luminosity or distance independent way If the uploaded photometry table includes also columns reporting the photometric errors in each band it is possible to select weather the software should consider these errors in the fit or to neglect photometric errors and treat the photometry as a individual points for each star Practically not considering the photometric errors corresponds to assigning a constant identical error to every magnitude or color If the photometric errors are used a further options allows to activated a Monte Carlo MC simulation to derive the errors in each derived stellar parameter for the individual sources This step is quite time consuming however it is needed to allow for a reliable estimate of the uncertainties since in general the measured photometric errors lead to highly c
18. e 2 4 the user must provide a 3 column ASCII table containing in this order values of Tog in K logg in cgs units and stellar radii R in units of Ro These 3 parameters are sufficient to perform synthetic photometry see Section 2 and compute absolute magnitudes or fluxes however stellar masses and ages will not be defined Note unlike magnitudes stellar colors are independent on luminosity therefore on stellar radius If user aims only at the analysis of stellar colors the values of stellar radii specified in Evolutionary Models Do you want to use evolutionary models or an arbitrary set of parameters C Arbitrary C all isochrones C alltracks manual input Evolutionary model Palla amp Stahler 1999 one isochrone one track 1111 rows oo Col 1 LogT 9 thisis a curve Z Col 2 LogL Lsun xj thisis a 2D grid L 7 E TA DA Tool for Astrophysical Data Analysis crims Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fitter Submit mu ol Figure 2 2 Importing an arbitrary table of 2 stellar parameters parameter 2 parameter 1 parameter 2 parameter 1 A parameter 2 c c c c c c c cce c ce parameter 2 parameter 1 parameter 2 Gun OK ee e parameter 2
19. elected star to the clicked point a popup windows is created showing the stars photometry and the location of this star in the uploaded table 15 TA DA User data table 3 bal catalog_table_NEW dat found 14 columns and 2621 lines showing lines 10 100 a previous page cument page 1 next page gt last page gt gt 1523 selected F n icol2 col3 icol4 col7 col8 col9 col10 sort selection sort sort sot sot sot sot sot sot sot sot none al notused v notused fnotused y er WFILU y er WFILB y 1620 Eli 01 05 17 56 9 9 999 12 097 0002 05735720 71 057217444 0 008 9 540 0535 05 20 05714 50 3 10 535 4 05734714 16 05736754 1 9 929 x 05735721 31 05712 127 10 646 ler WEI 05 35 2841 05 26 201 ler 1 a 05734711 11 05722546 0 018 x 0573474997 05718 446 0 023 a 05735716 72 057237252 0 019 4 05734739 75 057247256 0 021 4 05735716 937 05721 454 0 015 lt a 05735749 79 05740727 8 0 010 c 05734720 10 05738758 5 0 012 x 05734715 18 05711 494 0 017 a 05735705 63 05725719 4 0 012 4 0573572021 05720757 0 0 010 4 0573575045 05728734 8 0 020 x 05735743 15 05720713 8 b 0573571733 05722 45 4 13 208 a 05734755 37 4057237130 12 883 05735710 72 0572374446 15 088
20. es Settle 2002 name of the grid PARN 3 number of model parameters WAVN 1221 number of wavelength points WAVUNIT Angstrom units of wavelength scale PARNAME1 T name of first parameter PARNAML1 Temperature name of first parameter long PARUNIT1 K units of first parameter PARMIN1 1100 00 minimum value of first parameter PARMAX1 2300 00 maximum value of first parameter PARNAME2 logg name of second parameter PARNAML2 Surface gravity name of second parameter long PARUNIT2 1og cgs units of second parameter PARMIN2 4 50000 minimum value of second parameter PARMAX2 5 50000 maximum value of second parameter PARNAME3 M H name of third parameter PARNAML3 Metallicity name of third parameter long PARUNIT3 log ratio units of third parameter PARMIN3 1 00000 minimum value of third parameter PARMAX3 0 000000 maximum value of third parameter MODN 52 number of model spectra Here I present an example of IDL code to produce a model grid It is assumed that the 5 variables lambda teff logg metallicity and spectra are already stored in IDL as arrays filename your path synthetic_grid fits FXHMAKE hdr EXTEND FXWRITE filename hdr FXBHMAKE newhdr 1 FXBADDCOL c1 newhdr lambda FXBADDCOL c2 newhdr teff FXBADDCOL c3 newhdr logg FXBADDCOL c4 newhdr metallicity FXBADDCOL c5 newhdr spectra FXADDPAR
21. flip Y axis 0017 05 35 we 10 043 0 020 1015 0018 05735 10 049 0 015 Wodata C 1 0019 05735 239143 min X WFILV wrt max X 3 91294 axis paas 0019 F 0020 05 34 10 064 0 017 157 R 0021 o5 l 81 TA DA Selected star info S leia F 0022 057351 INFORMATION ON THE CLICKED STAR Select the fat lines on the curent Entry number in the original uploaded table 915 here 1 is the first data row Current location on the TA DA User data table widget page 10 row 15 User defined IDL logical sting er wiv k F r foz cola 0573571090 057227464 99 999 wru 3 999 fer wr uU 99 999 3399 fer WFE er VFLV 16 860 0 049 IWFI_TI620 16 554 er_WFI_TI620 WF 0 029 15 005 fer WF 0 009 Figure 2 9 Example of the plotting window showing both TADA computed models and the user photometry 17 Panel 4 The stellar parameter fitter The photometry fitter included in TA DA allows one to derive the stellar parameters of the individual stars selected in the attached table This is a universal fitter and can be used in different scenarios based on the type of models on which synthetic photometry is performed the number of photometric bands of the measured photometry and the options declared in the fitter panel In general we distinguish two cases 1 Interpolation of evolutionary models and extinction if the number of free pa rameters is equal to the d
22. hecks the validity of the model points and moves to the next panel Panel 2 Synthetic Photometry In the second panel of TA DA the user can define all the necessary ingredients to perform synthetic photometry on the previously defined grid of grid of stellar models An example of the layout of this panel is shown in Figure 2 5 e Selection of the synthetic model grid a drop down menu lists the available grids of synthetic spectra These are contained as fits table files in the subdirectory tada_data spectra within the TA DA installation directory When TA DA is launched the content of this di rectory is explored and the information on each data cube of spectra is read Thus the user can add additional grids of atmosphere models besides the defauld ones provided that they are saved in the proper format and copied in the appropriate directory Each grid can contain stellar spectra as a function of 3 parameters The first two are Ter and log g the third can be an arbitrary additional quantity such as metallicity or any arbitrary parameter The information on this parameter as well as its range are stored in the header 10 E TA DA Tool for Astrophysical Data Analysis Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fitter Compute synthetic spectra and photometry Select the photometric bands to perform synthetic photometry Atm
23. imension of the measured photometry space an exact solution can be obtained potentially of each source Some examples are a Interpolation in the CMD the synthetic photometry is computed for a number of isochrones or tracks the data include 2 photometric bands and the extinction is a fixed parameter the software will assign age and mass to the individual sources b Dereddening onto one isochrone the synthetic photometry is computed for a single g y y 8 isochrones 2 observed magnitudes or colors are provided the extinction is a free parameter the software will determine the amount of reddening and the de reddened position along the isochrone for each star c Determination of 2 stellar parameters e g mass and age or Tyg and log L as well as extinction for each star based on 3 magnitudes or 3 colors 2 Probabilistic SED fitting if the number of measured magnitudes or colors exceeds that of the free parameters the best fit solution for the parameters of each star is provided This approach is analogous to a general spectral energy distribution SED fitting proce dure in which extinction can be either constrained of left as a free parameter and the user can decide whether to consider only the shape of the SED or also the actual luminosity fitting photometric colors or photometric magnitudes g Figure 9 shows an example of the fitter panel From the top of the panel the user selects which photometric ban
24. le quantiy to ft magnitudes colors V use photometric eros Select file name Ji TADAS gt example input files Av 0000000 z Rv 210000 leave reddening as a fe parameter min Av 00 maxAv 100 step Av E save resul choose the format forthe output same number of row as in the uploaded table 6 soting as in the uploaded table only selected stars same sorting asin the current table view Name Date modified Z 2MASS PSCxml 11 9 2011 529 PM D big togt Jogl bt 11 7 2011 4 48 PM L catalog table NEW dat 4 1 2009 6 46 PM E mass agett 3 17 2011 1035 PM DD 3 15 2011 10 91 PM Type XML Document Text Document DAT File Text Document Text Document Filename TA DA fitter results bt Save as type 77 39 Hide Folders Figure 2 12 Interface to save the fitting results 22 Appendix Filter profiles The current version of TA DA includes the following filter profiles located in the folder tada_data throughputs 2MASS H COUSINS_R NIRCAM F410M WFC3UVIS_F225W WFC3UVIS_FQ619N 2MASS_J GALEX_FUV NIRCAM F418N WFC3UVIS_F275W WFC3UVIS_FQ634N 2MASS KS GALEX_NUV NIRCAM F430M VVFC3UV15 F280N WFC3UVIS_FQ672N ACSHRC F220VV IRAC_I1 NIRCAM_F444W WFC3UVIS_F300X WFC3UVIS_FQ674N ACSHRC_F250W IRAC_I2 NIRCAM
25. ly of models d one track The user specifies one value of mass in solar masses TA DA interpolates the evolutionary models to that value of mass if within the parameter range spanned by the models e manual input Selecting this option the user specifies an arbitrary set of stellar parameters this is passed to the software through an ASCII text file selected through a popup window The ASCII file must contain 2 columns or more in which case only the two are considered which contain any combination of the following parameters a mass Mo b age Myr c log Teg K d log bo Lo e R Ro The type of parameter described in each column must be manually specified through 2 drop lists in the widget GUI The remaining 3 parameters as well as the surface gravity log g are interpolated by the TA DA from the considered evolutionary models TA DA also checks that the user provided parameter grid lies inside the parameter space covered by the evolutionary models If this condition is not matched for a fraction of the points an warning message is generated and the software neglects these points If all the specified points lie outside the evolutionary model grid an error is generated and the user is asked to modify the input parameters Finally the user must specify wether the parameters provided through the ASCII file represent a 1 dimensional curve or a 2 dimensional grid In the latter case the grid must be rectilinear
26. minosity therefore on stellar radius If user aims only at the analysis of stellar colors the values of stellar radii specified in the 3rd column of the ASCII file can be arbitrary for example 1 R for every model point When the user defines which column is associated to any photometric band previously used for performing synthetic photometry and some stars rows are selected in the table window the plot window is automatically updated showing together with the computed models the observed photometry of the selected stars An example of this is shown in Figure 8 in this example the plot window shows a 2 color diagram computed in the bands WFI V WFI I and WFI_Ti620 and the attached table provides photometry in these and other bands obtained in the Orion Nebula Cluster Da Rio et al 2009 The models indicate with different colors represent the synthetic photometry in these bands for different Palla amp Stahler isochrones When at least 2 photometric bands are specified in the table window and at least one star is selected in the TA DA main window the button go to the fitter is activated Clicking on this button produces a fourth panel in the TA DA main window with a list of options to perform the fit of the models on the attached data Clicking on the plot window A mouse click on the plot window provides information on both stars and model points located in that point of the plot e A left click is for the closest s
27. nd options Particularly large sets of model points may require some time e g a full set of stellar masses and ages counting 100 000 model points for 6 values of reddening and 6 photometric bands requires about 15 minutes of computing time on an average desktop computer During the computation the approximate progress in percentage is shown Panel 3 Results of synthetic photometry and plots After the synthetic photometry is computed the software moves to the third panel see Figure 2 6 Here a brief summary of the results is present The synthetic photometry is natively 12 E TA DA Tool for Astrophysical Data Analysis m H 2 Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fitter SUMMARY You can now upload a table containing your photometry Number of model points 40587 Select ascii table N column or VOTable xml successful synthetic photometry 40587 P unsuccessful synthetic photometry 0 E TA DA Plot window x parameters not covered by evolutionary models 0 Teff not covered by atmosphere models 0 log a not covered by atmosphere models 0 5 29625 Av 0 000000 y Rv 3 10000 Export postscript maxY Select the units to express the synthetic photometry These wil be considered forthe next steps igi m O MODEL POINT INFORMATION C erp s em 2 A C A 3 54869 Vegamag WFI_TI6 7116 Vegamag Save synthetic phot
28. nitudes and colors are computed in a number of units Dust extinction can be considered in the computation 2 The results of synthetic photometry are plotted for visual inspection and can be saved to file 3 Tables with observed photometry can be imported in the program The individual entries in the imported table can be sorted and selected The data are plotted in comparison with the synthetic photometry 4 A universal fitting algorithm is used to derive the best stellar parameters of individual sources based on the their magnitudes or colors and associated photometric errors in an arbitrary number of simultaneous bands up to 16 1 3 Installation The program is available as a pre compiled IDL application TA DA can be obtained from the following URL http www rssd esa int SA general Projects Staff ndario TADA index html as a compressed archive tada zip The archive content is the following e the file tada sav the pre compiled IDL code the directory tada data contains the necessary data for the program to run e g the synthetic spectra the filter profiles some family of theoretical isochrones e the directory example_input_files contains examples of input files that can be imported to data for testing To install TA DA it is sufficient to decompress the archive and run the program tada sav from IDL IDL gt cd path where tada is located IDL gt tada Note the user may conside
29. nts 1 mtroduction ii A e tanta ere a el artes 1 TT What is TA DA coi a ee aa sa ee a A ee a 1 1 27 TADA Tunctionaliti s ec fe AS ee A A 8 1 1 3 Installation oes wie A E ed eee en ee BAe 2 1 4 Compatibility tas ee A bre ee Ge ot AS a 3 2 Using TADA ui ide ies x p ae a Sen aa MER os Owe R d fo oR cs Be he vs 5 2 1 Panel 1 Physical stellar parameters for the model 5 2 1 1 Evolutionary Models 5 2 1 2 No evolutionary models defining only Teg logg 2 7 Panel 2 Synthetic Photometry 9 Panel 3 Results of synthetic photometry and plots 11 Panel 3 Uploading photometric data 13 Clicking on the plot window e 14 Adding labels to epot ninia eg m ee ere 15 Panel 4 The stellar parameter fitter 0 0 0 0 0 0 1010 0 0 17 Models and Filters s a ae a a Boe R r s 23 Eilter profil s 2 00 i202 oe Sen ee does Sa oe ene 23 Evolutionary models se ee ee a a a ee 24 DYyNthetic Specthar s tn tte Ae accuse Sete tela doe Gan 26 29
30. ometry to file E ari Save fiters information to file 0 Tef 3102 log L 1 02388 log Lsun R 1 06831 Rsun log a 3 59121 log egs WFI_TI620 2 min Y 23 6894 flip Y axis 4 H m x vexX i38275 fip axis 0 291492 min X wri v Figure 2 6 TA DA panel with the results of synthetic photometry and plotting window The small window on the top right corner is the model point information generated by right clicking on a point of the plot see below 13 computed in units of VegaMag magnitudes calibrated using a flux calibrated spectrum of Vega Bohlin et al 2007 However the program derives all the conversions to express the results in units of ABmag or STmag magnitudes as well as flux either Jansky or erg s cm A m the third panel it is possible to switch from one to another units The results of synthetic photometry in the chosen units can be saved to a file through an apposite button This will be an ASCII table in which every row represents one model point The columns report all the stellar physical parameters as well as Ay and the magnitudes or fluxes From panel 3 with the button Save filters information to file the saves a file with the information about the selected photometric bands This includes effective wavelength central wavelength equivalent width and the zero points in Jansky and erg s cm A Such information may be useful when ne
31. orrelated and non linear errors in the model parameter space Finally the user can select whether to fix a single value of Ay for every star or to leave the reddening as a free parameter to be derived by the fitter star by star In this latter case a range of extinction values and a first order resolution is specified Important note in order to leave reddening as a free parameters at least 2 distinct values of Ay must have been specified earlier when the synthetic photometry was performed Panel 2 By clicking on the button run fitter the parameter fitting algorithm processes each se lected star of the user data table Data outside the model predicted space In both the cases introduced above interpolation and exact solution or probabilistic approach it is possible that stars show observed magnitude or colors which are incompatible with the predictions from the synthetic photometry on the evolutionary models As an example one could consider a star located just below the main sequence on a CMD In these cases TA DA still provides the most probable solution which is the closest point to the observed fluxes and within the theoretical magnitude space in the direction of the photometric errors This is illustrated in Figure 2 11 Along with the estimated parameters for each source the results of the fitter provide the distance in units of photometric error sigma from the observed fluxes to the those of the most probable solution
32. osphere models NextGen Y instrument system WFI x band Ju y Metalicty l validrange 1 5t0 0 instrument system WAI Elba l El F extrapolation for log a values outsidethegid instrament system FI zi bana v 21 instrument system WEI band T1620 Include extinction in the models instrument system WEI z b ndli y reddening law Cardeli 1989 instrument system NIRCAM band FO70W Y add one band remove band Av 0 0 1 2 one or more values comma separated FO7OW FOSOW Rv 3 1 5 5 one or more values comma separated EW F150W F150W2 F162M Distance modulus 8 085 F182M F187N F210M F212N F225N F250M F277W il F300M F322V 2 F323N F335M F356W F360M FADSN F410M FA18N F430M FAAAVI F460M Submit F466N F470N Help Qut FAB M d Figure 2 5 TA DA second panel input parameters for the synthetic photometry of the fits table and automatically considered by TA DA For additional instructions on the format of the synthetic spectra cubes see the appendix at the end of this manual Extrapolation of log g this option allows the user to choose how TA DA should consider model points with a surface gravity logg outside the parameter range convered by the selected grid of atmosphere models If the option is deactivated any point of the stellar parameters defined in panel 1 with a log g value outside the range spanne
33. r adding the directory where the program is located is added to the IDL path although this is not necessary When TA DA is started it creates a widget based interface This is divided in 4 tabs one for each main step of the analysis performed by the software 1 The interpolation of evolutionary models 2 the synthetic photometry 3 the results of synthetic photometry the plotting and the uploading of the photometric data and 4 the fitter engine 1 4 Compatibility TA DA has been developed to work under IDL version 7 0 or higher on all Windows Linux or Mac OS platforms The widget based graphical user interface however looks and behaves best under Windows systems This is because IDL widgets allow more strict positioning and sizes under Windows Chapter 2 Using TA DA 2 1 Panel 1 Physical stellar parameters for the model The first panel is dedicated to the preparation of the model stellar parameters for synthetic photometry TA DA allows two general approaches for this step which can be switched from the top row of Panel 1 see also Figure 2 1 1 Evolutionary models this approach considers evolutionary models evolutionary tracks and isochrones In this way the stellar parameters include besides the effective temper ature Teg the stellar radius R and the surface gravity logg parameters necessary for synthetic photometry also stellar masses M and stellar ages 2 Arbitrary this approach considers only
34. rid The results of the fit can be saved to an ASCII table either preserving the same row to row correspondence of the imported data table or just limited to the selected source 20 TA DA Tool for Astrophysical Data Analysis m Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fiter Stellar parameters fitter Select the photometric bands to use ToweLU Fo Well M WFB IV WFI_TI620 M NIRCAM_F150W Observable quantity to fit magnitudes colors V use photometric emors MC simulation of uncertainties constrain reddening Av 0 000000 x Fv 3 10000 7 leave reddening as a free parameter min Av 0 0 max Av 5 0 step Av 0 5 Rv 3 10000 processing star 10 of 2621 Figure 2 10 Example of the Parameters Fitter panel data point outside grid most likely solution mag2 mag1 Figure 2 11 Schematic representation of the best parameter fitting technique a probabilistic approach when the observed data are outside the range spanned by the models a and an exact interpolation otherwise b 21 TA DA Tool for Astrophysical Data Analysis Evolutionary Models Synthetic Photometry Synthetic photometry resuts Parameter fiter Stellar parameters fitter Select the photometric bands to use wr M WEI_TI62O Wwe 9 TT NIRCAMLF150W Observab
35. s additional examples are present in the file itself 16 TA DA User data table Se 2MASS PSC xl found 17 columns and 2844 Ines showing ines 110 100 Tia selected CREATED TV RAJ2000 DpE 2000 rwomass IMAG Esmas amas E HMAG KMAG E kmaG iris RFLG BFLG cria XFLG AFLG 2 sot selection sti so st st sot sto s t sot sto so sot sot sot sot sot rore a rot used not used Y not used not used rotused xl not used not used y not used x rot used E ver 83 735004 56347910 05345640 05381 127560 1010240000 12 0900 1010330000 1113590 0023000 AAA 22 m 000 201 1110 Maer 83 745961 5 6307640 105345903 0527 13 9590 010260000 130130 0103000100 1255110 0010260000 AAA 22 m 000 T 2011 1110 VizeR 83 741750 56329920 05345802 05377 14 6990 0 0320000 135690 0103500100 130180 00210000 AAA 22 m 000 201 1110 VizeR 83692057 5 6253430 _05344609 053713 6490 010240000 123400 00310000 126190 010230000 AAA 222 m 000 T 2011110 VizeR 83 742753 56404780 0534582605382 13 7930 00280000 1122340 0 0330000 11 5230 0102300100 AAA 22 m s n 2011 41110 VizeR 83 762486 5 6446020 05350239 05384 14 8160 0 340000 142770 00410000 138770 00350000 AAA 222 m 000 T 201110 VizeR 83 750175 5 6374880 05350004 0538118 7760 010340000 164720 0 041000 136430 0 0300000 UUA 002 001 000 F 20011110 Maier 83 755910 56497650 05350147 0538 15 3810 00440000
36. the minimum parameters to perform synthetic photometry i e Ter R and logg Stellar masses and ages which are model dependent quantities will be undefined 2 1 1 Evolutionary models When selecting the evolutionary model approach the panel shows additional widgets see e g Figures 2 1 and 2 2 where the parameters must be specified Specifically the user selects the family of evolutionary models the available models are loaded automatically by TA DA at startup and additional families can be added see the appendix for details The user can then select among 5 options a all isochrones TA DA considers all isochrones from the selected family of models 5 TA DA Tool for Astrophysical Data Analysis Evolutionary Models Synthetic Photometry Synthetic photometry results Parameter fitter Do you want to use evolutionary models or an arbitrary set of parameters 9 Evolutionary Models Aibtra y Evolutionary model ALTERAN 1 00 y C allisochrones C one isochrone C alltracks one track 053 Msun manual input Help Qut Figure 2 1 Selection of the evolutionary models to use for synthetic photometry b one isochrones The user specifies one value of age in Myr TA DA interpolates the evolutionary models to that value of age if within the parameter range spanned by the models c all tracks TA DA considers all mass tracks from the selected fami
37. ugh a drop down menu for individual columns if a particular column reports the observed photometry or the associated photometric errors in one of the bands for which synthetic photometry is computed The software assumes the units are the same selected in Panel 3 of the main TA DA window The user table window also allows one to navigate through the table sort columns and select individual rows stars for further 14 analysis The selection can be performed manually by clicking to the left side of each row or automatically by selecting all the rows or the first n rows in a given page or the entire table or through and IDL logical expression En example of such expression could be the following johnson_v ge 10 and err_cousins_i lt 1 and col9 ne new meaning that the software will select all the rows for which the Johnson V magnitude is greater or equal than 10 mag the photometric error associated to the Cousins I photometry is less than 1 mag and the 9th column not associated any photometric band is not equal to the string new Note the automatic selections at the bottom of the table window selection by rows and by logical expression are additive stars that satisfy the input conditions are added to those previously selected If you want to select only the stars that satisfy the last condition you must deselect all the stars first using the apposite button Note unlike magnitudes stellar colors are independent on lu
38. w filters are added providing solely the filter throughputs At the completion of the synthetic photometry computation TA DA also creates a plotting window showing the results see Figure 2 6 One can select the quantities shown in the two axes choosing either colors or magnitudes and arbitrary ranges for each axis The units for each axis in the plot are automatically updated when the user changes the defaults units in Panel 3 If the selected units represent a flux i e Jansky or rg s cm A the color terms will be the ratio instead of the difference between the fluxes in the 2 selected filters Panel 3 Attaching photometric data From the right hand part of panel 3 the user can attach a table containing observational data to TA DA This is expected to contain multiple rows one for each star and multiple columns providing photometry or additional data relative to each source This generates a new widget window showing the content of the table as well as a number of widgets to explore and organize its content select individual sources etc Supported formats are either ASCII table or XML VOtable The format as well as the number columns and rows of the attached table are auto matically detected by TA DA Figure 2 7 and 2 8 show two examples of the result respectively for an ASCII and a VOTable If the attached table is a VOtable the original names of the fields columns are shown In any case the user must specify manually thro
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