Models for dynamically dissolving star clusters (Kruijssen, 2009)

Details Models for dynamically dissolving star clusters (Kruijssen, 2009) Models for dynamically dissolving star clusters (Kruijssen, 2009)

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ycat..35071409k&link_type=abstract

VizieR On-line Data Catalog: J/A+A/507/1409. Originally published in: 2009A&A...507.1409K

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Models: Evolutionary, Associations: Stellar

Scientific paper

Evolutionary models for dissolving star clusters, computed with SPACEv3.0 (also see http://www.astro.uu.nl/~kruijs). The SPACE star cluster models contain evolution data for clusters with seven different metallicities. The set of data provided here contains models for five different dissolution timescales, three sets of remnant kick velocities, and two King profile parameters. 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 models are calculated for a Kroupa (2001MNRAS.322..231K) IMF, using the isochrones from the Padova group (Marigo et al., 2008A&A...482..883M). The initial-final mass relations for stellar remnants and other details are listed in the main paper.
The model parameters of each data set are summarised in the filenames of the data (K09NNNN.dat). For example, a filename K095201.dat gives the cluster evolution for a metallicity Z=0.02 ([Fe/H]=0.0), a dissolution timescale t0=3Myr, kick velocities that are 0.5 times the standard values {4,100,80} km/s for white dwarfs, neutron stars, and black holes (so {2,50,40} km/s), and a King profile parameter W0=7.
After the filename header "K09_", the meaning of the numbers is as follows.
The first number (0-6) indicates the metallicity: 0 - Z = 0.0001 ([Fe/H]=-2.3) 1 - Z = 0.0004 ([Fe/H]=-1.7) 2 - Z = 0.001 ([Fe/H]=-1.3) 3 - Z = 0.004 ([Fe/H]=-0.7) 4 - Z = 0.008 ([Fe/H]=-0.4) 5 - Z = 0.02 ([Fe/H]=0.0) 6 - Z = 0.03 ([Fe/H]=0.18)
The second number (0-4) indicates the dissolution timescale parameter t_0: 0 - t0= 0.3Myr (recommended for M51, Antennae) 1 - t0= 1Myr (recommended for the Galactic globular cluster system, though individual t_0 values show substantial scatter) 2 - t0= 3Myr (recommended for the solar neighbourhood, M33) 3 - t0= 10Myr (recommended for gas-poor spiral galaxies) 4 - t0= 30Myr (recommended for the SMC, LMC)
The third number (0-2) indicates the factor by which the standard kick velocities {4,100,80} km/s for white dwarfs, neutron stars, and black holes (WDs, NSs, BHs) are multiplied: 0 - 0.5 (i.e. {2,50,40} km/s for WDs, NSs, and BHs) 1 - 1 (i.e. {4,100,80} km/s for WDs, NSs, and BHs) - RECOMMENDED 2 - 2.5 (i.e. {10,250,200} km/s for WDs, NSs, and BHs)
The fourth number (0-1) indicates the King profile parameter W_0: 0 - W0= 5 (recommended for open clusters) 1 - W0= 7 (recommended for globular clusters)
The models are computed for initial cluster masses between 102 and 107M&sun;. If a certain initial mass does not appear in the list, this means that it was disrupted within 10Myr.
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]
(2 data files).

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