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On the Identification of N-rich Metal-poor Field Stars with Future Chinese Space Station Telescope

Research in Astronomy and Astrophysics 2024年第1期24卷 151-164页

作者： Jiajun Zhang baitian tang Jiang Chang Xiangxiang Xue JoséGFernández-Trincado Chengyuan Li Long Wang Hao Tian Yang Huang School of Physics and Astronomy Sun Yat-sen UniversityZhuhai 519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Sun Yat-sen UniversityZhuhai 519082China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210034China Key Lab of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Instituto de Astronomía Universidad Católica del NorteAv.Angamos 0610AntofagastaChile Key Lab of Space Astronomy and Technology National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China

During the long term evolution of globular clusters(GCs), some member stars are lost to the field. The recently found nitrogen-rich(N-rich) metal-poor field stars are promising candidates of these GC escapees, since N enhancement is the fingerprint of chemically enhanced populations in GCs. In this work, we discuss the possibility of identifying N-rich metal-poor field stars with the upcoming Chinese Space Station Telescope(CSST). We focus on the main survey camera with NUV, u, g, r, i, z, y filters and slitless spectrograph with a resolution about *** combination of UV sensitive equipment and prominent N-related molecular lines in the UV band bodes well for the identification: the color–color diagram of(u-g) versus(g-r) is capable of separating N-rich field stars from normal halo stars, if metallicity can be estimated without using the information on u-band ***, the synthetic spectra show that a signal-to-noise ratio of 10 is sufficient to identify N-rich field stars. In the near future, a large sample of N-rich field stars found by CSST, combined with state-of-the-art N-body simulations will be crucial to deciphering GC-Galaxy co-evolution.

关键词： stars:chemically peculiar stars:abundances techniques:photometric techniques:spectroscopic

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Driving factors behind multiple populations

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Science China(Physics,Mechanics & Astronomy) 2024年第5期67卷 172-181页

作者： Ruoyun Huang baitian tang Chengyuan Li Doug Geisler Mario Mateo Ying-Yi Song Holger Baumgardt Julio A.Carballo-Bello Yue Wang Jundan Nie Bruno Dias JoséG.Fernández-Trincado School of Physics and Astronomy Sun Yat-sen UniversityZhuhai 519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Zhuhai 519082China Departamento de Astronomía Universidad de ConcepcionConcepcionChile Instituto de Investigación Multidisciplinario en Ciencia y Tecnología Universidad de La SerenaLa SerenaChile Departamento de Astronomía Facultad de CienciasUniversidad de La SerenaChile Department of Astronomy University of MichiganAnn Arbor 48109USA David A.Dunlap Department of Astronomy&Astrophysics University of TorontoToronto ON M5S 3H4Canada Dunlap Institute for Astronomy&Astrophysics University of TorontoToronto ON M5S 3H4Canada School of Mathematics and Physics The University of QueenslandSt.Lucia QLD 4072Australia Instituto de Alta Investigación Universidad de TarapacáAricaChile CAS Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Instituto de Astrofísica Departamento de Ciencias FísicasFacultad de Ciencias ExactasUniversidad Andres BelloSantiagoChile Instituto de Astronomía Universidad Católica del NorteAntofagastaChile

Star clusters were historically considered simple stellar populations,with all stars sharing the same age and initial chemical ***,the presence of chemical anomalies in globular clusters(GCs),called multiple stellar populations(MPs),has challenged star formation theories in dense *** studies show that mass,metallicity,and age are likely controlling parameters for the manifestation of *** the limit between clusters with/without MPs in physical parameter space is crucial to reveal the driving mechanism behind their *** this study,we look for MP signals in Whiting 1,which is traditionally considered a young *** the Magellan telescope,we obtained low-resolution spectra withinλλ=3850-5500?for eight giants of Whiting *** measured the C and N abundances from the CN and CH spectral indices.C and N abundances have variations comparable with their measurement errors(~0.1 dex),suggesting that MPs are absent from Whiting *** these findings with literature studies,we propose a limit in the metallicity *** compactness index parameter space,which relatively clearly separates star clusters with/without MPs(GCs/open clusters).This limit is physically *** a larger scale,the galactic environment determines cluster compactness and metallicity,leading to metal-rich,diffuse,old clusters formed ex *** proposed limit also impacts our understanding of the formation of the Sagittarius dwarf galaxy:star clusters formed after the first starburst(age≤8-10 Gyr).These clusters are simple stellar populations because the enriched galactic environment is no longer suitable for MP formation.

关键词： stellar galactic galaxy

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Toward a stellar population catalog in the Kilo Degree Survey:The impact of stellar recipes on stellar masses and star formation rates

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Science China(Physics,Mechanics & Astronomy) 2023年第12期66卷 203-229页

作者： Linghua Xie Nicola R.Napolitano Xiaotong Guo Crescenzo Tortora Haicheng Feng Antonios Katsianis Rui Li Sirui Wu Mario Radovich Leslie K.Hunt Yang Wang Lin tang baitian tang Zhiqi Huang School of Physics and Astronomy Sun Yat-sen UniversityZhuhai 519082China CSST Science Center for the Guangdong-Hongkong-Macao Greater Bay Area Zhuhai 519082China Institute of Astronomy and Astrophysics Anqing Normal UniversityAnqing 246133China INAF—Osservatorio Astronomico di Capodimonte Napoli 80131Italy Yunnan Observatories Chinese Academy of SciencesKunming 650011China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China National Astronomical Observatories Chinese Academy of SciencesBeijing 100012China INAF—Osservatorio Astronomico di Padova Padova 35122Italy INAF—Osservatorio Astronomico di Arcetri Firenze 50125Italy Peng Cheng Laboratory Shenzhen 518000China School of Physics and Astronomy China West Normal UniversityNanchong 637002China

The Kilo Degree Survey(Ki DS)is currently the only sky survey providing optical(ugri)plus near-infrared(NIR,ZY H JKS)seeing matched photometry over an area larger than 1000 *** is obtained by incorporating the NIR data from the VISTA Kilo Degree Infrared Galaxy(VIKING)survey,covering the same Ki DS *** such,the Ki DS multi-wavelength photometry represents a unique dataset to test the ability of stellar population models to return robust photometric stellar mass(M_(*))and star-formation rate(SFR)*** we use a spectroscopic sample of galaxies for which we possess ugri ZY JHK_(s)“gaussianized”magnitudes from Ki DS data release *** fit the spectral energy distribution from the 9-band photometry using:(1)three different popular libraries of stellar population templates,(2)single burst,simple and delayed exponential star-formation history models,and(3)a wide range of priors on age and *** template fitting codes we use two popular softwares:Le Phare and *** investigate the variance of the stellar masses and the star-formation rates from the different combinations of templates,star formation recipes and codes to assess the stability of these estimates and define some“robust”median quantities to be included in the upcoming Ki DS data *** a science validation test,we derive the mass function,the star formation rate function,and the SFR-M_(*)relation for a low-redshift(z<0.5)sample of galaxies,that result in excellent agreement with previous literature *** final catalog,containing~290000 galaxies with redshift 0.01

关键词： galaxies stellar populations galaxy stellar masses star formation rates stellar mass function

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Searching for Multiple Populations in Star Clusters Using the China Space Station Telescope

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Research in Astronomy and Astrophysics 2022年第9期22卷 47-62页

作者： Chengyuan Li Zhenya Zheng Xiaodong Li Xiaoying Pang baitian tang Antonino P.Milone Yue Wang Haifeng Wang Dengkai Jiang School of Physics and Astronomy Sun Yat-sen UniversityDaxue RoadZhuhaiGuangdong 519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Zhuhai 519082China CAS Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryShanghai 200030China Division of Optical Astronomical Technologies Shanghai Astronomical ObservatoryShanghai 200030China Department of Physics Xi'an Jiaotong-Liverpool UniversitySuzhou 215123China Shanghai Key Laboratory for Astrophysics Shanghai Normal University100 Guilin Roadshanghai 200234China Dipartimento di Fisica e Astronomia“Galileo Galilei” Universitàdi PadovaVicolo dell'Osservatorio 31-35122PaduaItaly Istituto Nazionale di Astrofisica—Osservatorio Astronomico di Padova Italy Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 1001010China GEPI Observatoire de ParisUniversitéPSLCNRSPlace Jules Janssen F-92195MeudonFrance Yunnan Observatories Chinese Academy of Sciences396 YangfangwangGuandu DIstrictKuming 650216China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China

Multiple stellar populations(MPs) in most star clusters older than 2 Gyr, as seen by lots of spectroscopic and photometric studies, have led to a significant challenge to the traditional view of star formation. In this field, spacebased instruments, in particular the Hubble Space Telescope(HST), have made a breakthrough as they significantly improved the efficiency of detecting MPs in crowded stellar fields by images. The China Space Station Telescope(CSST) and the HST are sensitive to a similar wavelength interval, but the CSST covers a field of view which is about 5–8 times wider than that of HST. One of its instruments, the Multi-Channel Imager(MCI),will have multiple filters covering a wide wavelength range from NUV to NIR, making the CSST a potentially powerful tool for studying MPs in clusters. In this work, we evaluate the efficiency of the designed filters for the MCI/CSST in revealing MPs in different color–magnitude diagrams(CMDs). We find that CMDs made with MCI/CSST photometry in appropriate UV filters are powerful tools to disentangle stellar populations with different abundances of He, C, N, O and Mg. On the contrary, the traditional CMDs are blind to multiple populations in globular clusters(GCs). We show that CSST has the potential of being the spearhead instrument for investigating MPs in GCs in the next decades.

关键词： Galaxy:globular clusters general-stars abundances-techniques photometric

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