Photometric evolution of star clusters models (Kruijssen+, 2008)

Details Photometric evolution of star clusters models (Kruijssen+, 2008) Photometric evolution of star clusters models (Kruijssen+, 2008)

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008ycat..34900151k&link_type=abstract

VizieR On-line Data Catalog: J/A+A/490/151. Originally published in: 2008A&A...490..151K

Other

Models: Evolutionary, Clusters: Globular, Clusters: Open

Scientific paper

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 t0=10Myr.
In the files, columns are plotted for initial cluster masses between 102 and 107M{sun}
The absolute magnitudes of the Sun that have been used to convert luminosities to magnitudes are: [M{U,B,V,R,I,J,H,K}]=[5.61,5.48,4.83,4.42,4.08,3.64,3.32,3.28]
(7 data files).

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