========================================================================== J/A+A/490/151 Photometric evolution of star clusters models (Kruijssen+, 2008) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat Z0004/* Z004/* Z008/* Z02/* Z05/* ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/490/151 ==========================================================================
drwxr-xr-x 14 cats archive 4096 Jan 29 2012 [Up] drwxr-xr-x 7 cats archive 4096 May 12 09:57 [TAR file] -rw-r--r-- 1 cats archive 503 Nov 17 2009 .message -r--r--r-- 1 cats archive 10387 Dec 31 2008 ReadMe drwxr-xr-x 2 cats archive 4096 Nov 17 2009 Z0004 drwxr-xr-x 2 cats archive 4096 Nov 17 2009 Z004 drwxr-xr-x 2 cats archive 4096 Dec 31 2008 Z008 drwxr-xr-x 2 cats archive 4096 Dec 31 2008 Z02 drwxr-xr-x 2 cats archive 4096 Dec 31 2008 Z05 -rwxr-xr-x 1 cats archive 743 Nov 17 2009 get_model -r--r--r-- 1 cats archive 191540 Nov 17 2009 models.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 578 Oct 9 2008 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/A+A/490/151 Photometric evolution of star clusters models (Kruijssen+, 2008) ================================================================================ The photometric evolution of star clusters and the preferential loss of low-mass stars with an application to globular clusters. Kruijssen J.M.D., Lamers H.J.G.L.M. <Astron. Astrophys. 490, 151 (2008)> =2008A&A...490..151K ================================================================================ ADC_Keywords: Models, evolutionary ; Clusters, globular ; Clusters, open Keywords: Galaxy: globular clusters: general - Galaxy: open clusters and associations: general - galaxies: star clusters - galaxies: stellar content - methods: numerical Abstract: To obtain an accurate description of broad-band photometric star cluster evolution, certain effects should be accounted for. Energy equipartition leads to mass segregation and the preferential loss of low-mass stars, while stellar remnants severely influence cluster mass-to-light ratios. Moreover, the stellar initial mass function and cluster metallicity affect photometry as well. Due to the continuous production of stellar remnants, their impact on cluster photometry is strongest for old systems like globular clusters. This, in combination with their low metallicities, evidence for mass segregation, and a possibly deviating stellar initial mass function, makes globular clusters interesting test cases for cluster models. In this paper we describe cluster models that include the effects of the preferential loss of low-mass stars, stellar remnants, choice of initial mass function and metallicity. The photometric evolution of clusters is predicted, and the results are applied to Galactic globular clusters. The cluster models presented in this paper represent an analytical description of the evolution of the underlying stellar mass function due to stellar evolution and dynamical cluster dissolution. Stellar remnants are included by using initial-remnant mass relations, while cluster photometry is computed from the Padova 1999 isochrones. Description: The SPACE star cluster models contain evolution data for clusters with five different metallicities, two stellar initial mass functions, with/without stellar remnants, with/without the preferential loss of low-mass stars, and three different dissolution timescales. Models for a wider range of parameters and for other observables can be made on request. Please send me an e-mail if you are interested. The model parameters of each data set are indicated by the filename, KNNNN_NN.dat, in five directories, Z0004, Z004, Z008, Z02 and Z05. The first number (0-4) indicates metallicity: 0 = Z=0.0004 ([Fe/H]=-1.7) 1 = Z=0.004 ([Fe/H]=-0.7) 2 = Z=0.008 ([Fe/H]=-0.4) 3 = Z=0.02 ([Fe/H]=0.0) 4 = Z=0.05 ([Fe/H]=0.4) The second number (0-1) indicates IMF: 0 = Salpeter 1 = Kroupa The third number (0-1) indicates whether stellar remnants are included: 0 = no remnants 1 = including remnants The fourth number (0-1) indicates whether the preferential loss of low-mass stars is included: 0 = no preferential loss of low-mass stars 1 = including the preferential loss of low-mass stars The last two numbers (after the underscore) indicate the dissolution timescale t_0 in Myr: 01 = t_0=1Myr 03 = t_0=3Myr 10 = t_0=10Myr For example, file Z02/K3101_10.dat gives cluster evolution for a metallicity Z=0.02 ([Fe/H]=0.0), a Kroupa IMF, no stellar remnants, including the preferential loss of low-mass stars and a dissolution timescale t_0_=10Myr. In the files, columns are plotted for initial cluster masses between 10^2^ and 10^7^M_sun_ The absolute magnitudes of the Sun that have been used to convert luminosities to magnitudes are: [MU,B,V,R,I,J,H,K]=[5.61,5.48,4.83,4.42,4.08,3.64,3.32,3.28]
© UDS/CNRS