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J/MNRAS/432/2746 POPSTAR models. III. Young star clusters (Garcia-Vargas+, 2013)

POPSTAR evolutionary synthesis models. III. Photometric properties of young star clusters and mixed populations. Garcia-Vargas M.L., Molla M., Martin-Manjon M.L. <Mon. Not. R. Astron. Soc., 432, 2746-2772 (2013)> =2013MNRAS.432.2746G
ADC_Keywords: Models, evolutionary ; Photometry ; Colors Keywords: H II regions - galaxies: abundances - galaxies: evolution - galaxies: starburst - galaxies: star clusters: general - galaxies: stellar content Abstract: This is the third paper of a series reporting the results from the POPSTAR evolutionary synthesis models. The main goal of this work is to present and discuss the synthetic photometric properties of single stellar populations resulting from our POPSTAR code. Colours in the Johnson and Sloan Digital Sky Survey (SDSS) systems, Hα and Hβ luminosities and equivalent widths, and ionizing region size, have been computed for a wide range of metallicity (Z=0.0001-0.05) and age (0.1Myr to 20Gyr). We calculate the evolution of the cluster and the region geometry in a consistent manner. We demonstrate the importance of the contribution of emission lines to broader band photometry when characterizing stellar populations, through the presentation of both contaminated and non-contaminated colours (in both the Johnson and SDSS systems). The tabulated colours include stellar and nebular components, in addition to line emission. The main application of these models is the determination of physical properties of a given young ionizing cluster, when only photometric observations are available; for an isolated star-forming region, the young star cluster models can be used, free from the contamination of any underlying background stellar population. In most cases, however, the ionizing population is usually embedded in a large and complex system, and the observed photometric properties result from the combination of a young star-forming burst and the underlying older population of the host. Therefore, the second objective of this paper is to provide a grid of models useful in the interpretation of mixed regions where the separation of young and old populations is not sufficiently reliable. We describe the set of popstar spectral energy distributions (SEDs), and the derived colours for mixed populations where an underlying host population is combined in different mass-ratios with a recent ionizing burst. These colours, together with other common photometric parameters, such as the Hα radius of the ionized region, and Balmer line equivalent widths and luminosities, allow one to infer the physical properties of star-forming regions even in the absence of spectroscopic information. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 56 4116 Computed radii for the modelled stellar clusters of all ages and metallicities, for ne=10 and 100cm-3 table4.dat 110 6216 Johnson colours evolution results for the modelled stellar clusters of all ages and metallicities, for ne=10 and 100cm-3 table5.dat 114 6216 SDSS colour evolution results for the modelled stellar clusters of all ages and metallicities, for ne=10 and 100cm-3 list.dat 43 198 List of tables in subdirectory "models" giving the evolution of clusters with 2 populations models/* 222 198 Individual files for each combination of 6 metallicities and 33 ages for the old stellar population (table 6) table6.zip 512 225425 All tables included in the subdirectory "models" and listed in list.dat
Description of file: table6.zip table6.zip includes all the files listed in list.dat and available individually in the subdirectory "models". We have calculated the colours of a system composed of two populations: one older than 100Myr (logτ(yr)≥8.00) and one younger than this same limit (logτ<8.00). The stellar mass of the young population in this model grid takes the same values as in the SSP models: 0.12, 0.20, 0.40, 0.60, 1.0, 1.5 and 2.0 x105M. For each model or composite system, we assume an old stellar population with a mass on the zero time main sequence defined by a factor F=Mold/Myoung. We have taken 6 possible values for this grid, F=0, 1, 10, 100, 1000 and 5000. Colours are computed by using the total luminosity emitted by both the old population and the young stellar population, including the emission lines contribution and the nebular continuum. We have obtained a table for each old stellar population defined by its age and metallicity, where all possible combinations with the young stellar population (scanning the grid in mass, age and metallicity of the young cluster) are included. table6.zip is a zip file with all these tables (198 files, 33 ages for each of the six metallicities). See section 4 for further explanations. See also: J/MNRAS/403/2012 : PopStar II. Giant HII regions models (Martin-Manjon+, 2010) J/MNRAS/398/451 : PopStar I: Evolutionary synthesis models (Molla+, 2009) J/A+A/471/795 : Population ages & metallicities from colors (Li+, 2007) J/A+A/428/837 : HII regions in minor mergers of galaxies (Ferreiro+, 2004) J/AJ/108/1276 : Clusters in GEHRs (Mayya, 1994) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 cm-3 ne [10/100] Electron density of the stellar cluster ISM used for CLOUDY models (10 or 100) 6- 11 F6.4 --- Z [0.0001/0.05] Total abundance of the stellar cluster 13- 17 F5.2 [yr] logt [5/8] Log of age of the stellar cluster 19- 22 F4.1 10+4Msun Mass [1.2/20] Initial total cluster mass 24- 33 F10.5 pc Rin [4.7/445.3] Inner radius of the HII region 35- 45 E11.5 pc deltaR Shell thickness of the HII region 47- 56 F10.5 pc Rout [6/8597] External radius (observed) of the HII region
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 cm-3 ne [10/100] Electron density of the stellar cluster ISM used for CLOUDY models 7- 12 F6.4 --- Z [0.0001/0.05] Total abundance of the stellar cluster 14- 18 F5.2 [yr] logt [5/8] Log of the age of the stellar cluster 20- 25 I6 Msun Mass [12000/200000] Initial total mass in stars in the cluster 28- 32 F5.2 [10-7W] logLHb [31/40] Log of luminosity of the Hβ line in erg/s 34- 38 F5.2 [10-7W] logLHa [31/41] Log of luminosity of the Hα line in erg/s 40- 46 F7.3 mag VMagc [-14.192/-6.948] Absolute V-band magnitude including emission lines 48- 53 F6.3 mag U-Bc U-B color index including emission lines 55- 60 F6.3 mag B-Vc B-V color index including emission lines 62- 67 F6.3 mag V-Rc V-R color index including emission lines 69- 74 F6.3 mag R-Ic R-I color index including emission lines 76- 82 F7.3 mag VMag [-14.093/-6.948] V-band absolute magnitude (uncontaminated) 84- 89 F6.3 mag U-B [-1.413/-0.241] Johnson U-B color index 91- 96 F6.3 mag B-V [-0.255/0.466] Johnson B-V color index 98-103 F6.3 mag V-R [-0.093/0.523] Johnson V-R color index 105-110 F6.3 mag R-I [-0.147/1.051] Johnson R-I color index
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 I3 cm-3 ne [10/100] Electron density of the stellar cluster ISM used for CLOUDY 7- 12 F6.4 --- Z [0.0001/0.05] Total abundance of the stellar cluster 14- 18 F5.2 [yr] logt [5/8] Log of the stellar cluster age 20- 25 I6 Msun Mass [12000/200000] Initial total mass in stars in the cluster 28- 34 F7.1 0.1nm EWHb [-10.6/500.4] Equivalent width of the Hβ line in Å 36- 42 F7.1 0.1nm EWHa [-67.6/3412] Equivalent width of the Hα line in Å 44- 50 F7.3 mag gMagc [-13.921/-6.569] Absolute magnitude in g-band including emission lines 52- 57 F6.3 mag (u-g)c u-g color index including emission lines 59- 64 F6.3 mag (g-r)c g-r color index including emission lines 66- 71 F6.3 mag (r-i)c r-i color index including emission lines 73- 78 F6.3 mag (i-z)c i-z color index including emission lines 80- 86 F7.3 mag gMag [-13.535/-6.569] Uncontaminated absolute g-band magnitude 88- 93 F6.3 mag u-g [-0.731/0.751] SDSS u-g color index 95-100 F6.3 mag g-r [-0.431/0.345] SDSS g-r color index 102-107 F6.3 mag r-i [-0.366/0.437] SDSS r-i color index 109-114 F6.3 mag i-z [-0.652/0.678] SDSS i-z color index
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 6 F6.4 --- Z [0.0001/0.05] Metallicity 8- 12 F5.2 [yr] logt [8/11] Age of the old stellar population (log) 14- 43 A30 --- FileName Name of the table in subdirectory models
Byte-by-byte Description of file (# headlines): models/*
Bytes Format Units Label Explanations
2- 7 F6.4 --- Z.o Old stellar population metallicity 9- 13 F5.2 [yr] logt.o Age (logarithmic scale) of the old stellar population (τ) 15- 20 F6.4 --- Z.y Young stellar population metallicity 22- 26 F5.2 [yr] logt.y Age (logarithmic scale) of the young stellar population 28- 31 I4 --- F Ratio Mold/Myoung 33- 40 E8.2 Msun M.y Mass of the young stellar population 42- 48 F7.2 pc Rout The HII region outer (or photometric) radius 50- 54 F5.2 [10-7W] LHa Logarithm of the luminosity of Hα line 56- 62 F7.2 0.1nm EWHa The equivalent width of Hα in Å 64- 70 F7.3 mag Vc Magnitude V in the Johnson system corrected by the emission line contribution 72- 78 F7.3 mag (U-B)c Colour U-B in the Johnson system corrected by the emission line contribution 80- 86 F7.3 mag (B-V)c Colour B-V in the Johnson system corrected by the emission line contribution 88- 94 F7.3 mag (V-R)c Colour V-R in the Johnson system corrected by the emission line contribution 96-102 F7.3 mag (R-I)c Colour R-I in the Johnson system corrected by the emission line contribution 104-110 F7.3 mag V Magnitude V in the Johnson system without the emission line contribution 112-118 F7.3 mag U-B Colour U-B in the Johnson system without the emission line contribution 120-126 F7.3 mag B-V Colour B-V in the Johnson system without the emission line contribution 128-134 F7.3 mag V-R Colour V-R in the Johnson system without the emission line contribution 136-142 F7.3 mag R-I Colour R-I in the Johnson system without the emission line contribution 144-150 F7.3 mag gc Magnitude V in the SDSS system corrected by the emission line contribution 152-158 F7.3 mag (u-g)c Colour U-B in the SDSS system corrected by the emission line contribution 160-166 F7.3 mag (g-r)c Colour B-V in the SDSS system corrected by the emission line contribution 168-174 F7.3 mag (r-i)c Colour V-R in the SDSS system corrected by the emission line contribution 176-182 F7.3 mag (i-z)c Colour R-I in the SDSS system corrected by the emission line contribution 184-190 F7.3 mag g Magnitude V in the SDSS system without the emission line contribution 192-198 F7.3 mag u-g Colour U-B in the SDSS system without the emission line contribution 200-206 F7.3 mag g-r Colour B-V in the SDSS system without the emission line contribution 208-214 F7.3 mag r-i Colour V-R in the SDSS system without the emission line contribution 216-222 F7.3 mag i-z Colour R-I in the SDSS system without the emission line contribution
Acknowledgements: Mercedes Molla, <mercedes.molla( at )ciemat.es> References: Molla et al. Paper I. 2009MNRAS.398..451M Cat. J/MNRAS/398/451 Martin-Majon et al. Paper II. 2010MNRAS.403.2012M Cat. J/MNRAS/403/2012
(End) Mercedes Molla [CIEMAT], Emmanuelle Perret [CDS] 30-Jul-2013
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