FUV and NIR size of the HI selected low surface brightness galaxies  

作　　者：Cheng Cheng Wei Du Cong Kevin Xu Tian-Wen Cao Hong-Xin Zhang Jia-Sheng Huang Chuan He Zi-Jian Li Shu-Mei Wu Hai Xu YSophia Dai Xu Shao Marat Musin 

机构地区：[1]Chinese Academy of Sciences South America Center for Astronomy,National Astronomical Observatories,CAS,Beijing 100101,China [2]National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [3]Key Laboratory of Optical Astronomy,NAOC,20A Datun Road,Chaoyang District,Beijing 100101,China [4]CAS Key Laboratory for Research in Galaxies and Cosmology,Department of Astronomy,University of Science and Technology of China,Hefei 230026,China [5]School of Astronomy and Space Science,University of Science and Technology of China,Hefei 230026,China

出　　处：《Research in Astronomy and Astrophysics》2021年第3期251-260,共10页天文和天体物理学研究（英文版）

基　　金：supported by the National Key R&D Program of China(Grant 2017YFA0402704);by the National Natural Science Foundation of China(NSFC,Nos.11803044,11933003,11673028);sponsored(in part)by the Chinese Academy of Sciences(CAS),through a grant to the CAS South America Center for Astronomy(CASSACA);supported by the NSFC(Nos.U1931109 and 11733006);the Young Researcher Grant funded by National Astronomical Observatories,Chinese Academy of Sciences(CAS);the Youth Innovation Promotion Association,CAS。

摘　　要：How low surface brightness galaxies(LSBGs)form stars and assemble stellar mass is one of the most important questions related to understanding the LSBG population.We select a sample of 381 HI bright LSBGs with both far ultraviolet(FUV)and near infrared(NIR)observations to investigate the star formation rate(SFR)and stellar mass scales,and the growth mode.We measure the FUV and NIR radii of our sample,which represent the star-forming and stellar mass distribution scales respectively.We also compare the FUV and H band radius-stellar mass relation with archival data,to identify the SFR and stellar mass structure difference between the LSBG population and other galaxies.Since galaxy HI mass has a tight correlation with the HI radius,we can also compare the HI and FUV radii to understand the distribution of HI gas and star formation activities.Our results show that most of the HI selected LSBGs have extended star formation structure.The stellar mass distribution of LSBGs may have a similar structure to disk galaxies at the same stellar mass bins,but the star-forming activity of LSBGs happens at a larger radius than the high surface density galaxies,which may help to identify the LSBG sample from the wide-field deep u band image survey.The HI is also distributed at larger radii,implying a steeper(or not)Kennicutt-Schmidt relation for LSBGs.

关 键 词：Galaxies:evolution Galaxies:dwarf Ultraviolet:galaxies Galaxies:star formation 

分 类 号：P15[天文地球—天文学]