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[2016-1-4]:Using star clusters as a Rosetta Stone to study UV-upturn in early-type galaxies
2015-12-29  |  作者:  |  【  】 【打印】 【关闭

【学术报告】
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报告题目:Using star clusters as a Rosetta Stone to study UV-upturn in early-type galaxies
报告人:庞晓莹
报告人单位:国家天文台(NAOC),上海应用技术学院(SIT)
报告时间:2016年1月4日下午2:30
报告地点:小学校会议室
报告语言:中文
报告摘要:
UV-upturn is found in elliptical galaxies and early-type spiral bulges whose spectral energy distributions (SEDs) are found to be surprisingly increase to shorter wavelengths over the range 2000 to 1200 Å, in contrary to the expectation of an old stellar systems that are usually assumed to be dark in the FUV. During the last decades, many efforts have been made to find out ”culprits” of the UV-excess. Most of the candidate stars mentioned above originate in the cluster environment. Studies of SED evolution of star cluster may provide a clue on the origin of the candidate stars of UV-upturn. We present GalevNB (Galev for N-body simulations), an utility that converts fundamental stellar properties of N-body simulations into observational properties using the GALEV (GAlaxy EVolutionary synthesis models) package, and thus 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 of mainstream instruments/telescopes, such as HST, ESO, SDSS, 2MASS, etc.), and into spectra that spans from far-UV (90 Å) to near-IR (160 μm). We use GalevNB to investigate the secular evolution of SED and color-magnitude diagram of a simulated star cluster over a few hundred million years. With the results given by GalevNB we discover an 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, thermal pulsing asymptotic giant branch (TPAGB) stars, white dwarfs and naked helium stars.
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