Mid-infrared Period-Luminosity Relations of Gaia DR3 Long Period Variables  

作　　者：Xiaohan Chen Xiaodian Chen Licai Deng Shu Wang Tianlu Chen 

机构地区：[1]Department of Physics,College of Science,Tibet University,Lhasa 850000,China [2]Key Laboratory of Cosmic Rays(Tibet University),Ministry of Education,Lhasa 850000,China [3]CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [4]School of Astronomy and Space Science,University of the Chinese Academy of Sciences,Beijing 100049,China [5]Department of Astronomy,China West Normal University,Nanchong 637009,China [6]Institute for Frontiers in Astronomy and Astrophysics,Beijing Normal University,Beijing 102206,China

出　　处：《Research in Astronomy and Astrophysics》2024年第7期56-70,共15页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China(NSFC,Grant Nos.12173047,12322306,12003046,12233009,and 12133002);support from the Youth Innovation Promotion Association of the Chinese Academy of Sciences(no.2022055 and 2023065);support from the National Key Research and Development Program of China,grants 2022YFF0503404 and 2019YFA0405504。

摘　　要：Long period variable(LPV)stars are very promising distance indicators in the infrared bands.We selected asymptotic giant branch(AGB)stars in the Large and Small Magellanic Cloud(LMC and SMC)from the Gaia Data Release 3 LPV catalog,and classified them into oxygen-rich(O-rich)and carbon-rich(C-rich)AGB stars.Using the Wide-field Infrared Survey Explorer database,we determined the W1-and W2-band period-luminosity relations(PLRs)for each pulsation-mode sequence of AGB stars.The dispersion of the PLRs of O-rich AGB stars in sequences C'and C is relatively small,around 0.14 mag.The PLRs of LMC and SMC are consistent in each sequence.In the W2 band,the PLR of large-amplitude C-rich AGB stars is steeper than that of small-amplitude C-rich AGB stars,due to their more circumstellar dust.By two methods,we find that some PLR sequences of O-rich AGB stars in the LMC are dependent on metallicity.The coefficients of the metallicity effect areβ=-0.533±0.213 mag dex~1andβ=-0.767±0.158 mag dex~1for sequence C in W1 and W2 bands,respectively.The significance of the metallicity effect in W1 band for the four sequences is 2.2-3.5σ.Both of these imply that distance measurements using O-rich Mira may need to take the metallicity effect into account.

关 键 词：STARS VARIABLES general-stars distances-infrared STARS 

分 类 号：P145.2[天文地球—天体物理] P172.4[天文地球—天文学]