We present GalevNB （Galev for N-body simulations）, a utility that converts fundamental stellar properties of N-body simulations into observational properties using the GALEV （GAlaxy EVolutionary synthesis models） ...We present GalevNB （Galev for N-body simulations）, a utility that converts fundamental stellar properties of N-body simulations into observational properties using the GALEV （GAlaxy EVolutionary synthesis models） package, and allowing direct comparisons between observations and N-body simulations. It works by converting fundamental stellar properties, such as stellar mass, temperature, luminosity and metallicity into observational magnitudes for a variety of filters used by mainstream instruments/telescopes, such as HST, ESO, SDSS, 2MASS, etc., and into spectra that span the range from far-UV （90 A） to near-IR （160 ~tm）. As an application, we use Ga 1 evNB to investigate the secular evolution of the spectral energy distribution （SED） and color magnitude diagram （CMD） of a simulated star cluster over a few hundred million years. With the results given by GalevNB we discover a UV-excess in the SED of the cluster over the whole simulation time. We also identify four candidates that contribute to the FUV peak： core helium burning stars, second asymptotic giant branch （AGB） stars, white dwarfs and naked helium stars.展开更多
基金funded by the National Natural Science Foundation of China,Nos.11443001(XYP)and 11073025(RS)the funds of the National Natural Science Foundation of China,No.11503015+11 种基金Shanghai education committee,No.1021ZK 151009027-ZZyy 15104the talents introduction project of the Shanghai Institute of Technology,No.10120K156031-YJ 2014-05the Silk Road Project Team based at National Astronomical Observatories,Chinese Academy of Sciences(NAOC,http://silkroad.bao.ac.cn)funding by the German Research Foundation(DFG)grant OL 350/1-1partly supported through computational resources of SFB 881“The Milky Way System”(subproject Z2)at the University of Heidelberg,Germany,in particular the Milky Way supercomputer hosted and co-funded by the Jülich Supercomputing Center(JSC)the travel grants of the DFG grant OL 350/1-1support by the Chinese Academy of Sciences Visiting Professorship for Senior International Scientists,Grant Number 2009S1-5the“Qianren”special foreign experts program of China,both at NAOCfunded by the Ministry of Finance of the People’s Republic of China under the grant ZDY Z2008-2,has been used for simulations,as well as the smaller GPU clusters titan,hydra and keplerfunded under the grants I/80041-043 and I/84678/84680 of the Volkswagen Foundation at ARI/ZAH,University of Heidelberg,Germanyfinancial support from the National Science Foundation under Grant No.1412449STScI theory grant HST-AR12840.01-A
文摘We present GalevNB （Galev for N-body simulations）, a utility that converts fundamental stellar properties of N-body simulations into observational properties using the GALEV （GAlaxy EVolutionary synthesis models） package, and allowing direct comparisons between observations and N-body simulations. It works by converting fundamental stellar properties, such as stellar mass, temperature, luminosity and metallicity into observational magnitudes for a variety of filters used by mainstream instruments/telescopes, such as HST, ESO, SDSS, 2MASS, etc., and into spectra that span the range from far-UV （90 A） to near-IR （160 ~tm）. As an application, we use Ga 1 evNB to investigate the secular evolution of the spectral energy distribution （SED） and color magnitude diagram （CMD） of a simulated star cluster over a few hundred million years. With the results given by GalevNB we discover a UV-excess in the SED of the cluster over the whole simulation time. We also identify four candidates that contribute to the FUV peak： core helium burning stars, second asymptotic giant branch （AGB） stars, white dwarfs and naked helium stars.
