恒星形成与宁静S0星系的中性氢气体含量
The Neutral Hydrogen Gas Content of Star-forming and Quiescent S0 Galaxies
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中文总结 AI 辅助
本研究通过MaNGA样本比较恒星形成S0、宁静S0与旋涡星系的HI含量，发现SFS0s性质介于两者间但更似旋涡，且质量较低，表明其由低质量前身形成，而宁静S0s为独立群体。
中文摘要 AI 辅助
透镜状（或S0）星系中仍保持活跃恒星形成的（SFS0s）是星系中独特的过渡群体。我们研究了从阿帕奇点天文台邻近星系巡天（MaNGA）中识别出的透镜状星系样本的HI（21厘米）中性氢含量，这些星系已被分类为恒星形成或宁静（qS0s）。我们将这些群体相互比较，并与MaNGA中的恒星形成旋涡星系样本进行比较。我们发现，SFS0s的HI质量分数和HI缺失度介于宁静S0星系和恒星形成旋涡星系之间，但与旋涡星系最为相似。宁静S0星系的HI消耗时间远长于SFS0和旋涡星系，后两者的时间大致相似。我们还比较了三个群体的分子气体分数，结果显示三个群体中最低的是宁静S0星系，其次是恒星形成S0星系，然后是恒星形成旋涡星系。总重子质量的比较表明，样本中恒星形成S0星系的质量显著低于qS0s。这表明恒星形成S0星系必须由较低质量的前身（未被MaNGA观测到）形成，这些前身要么吸积外部气体，要么失去旋臂。质量更大的宁静S0星系是完全独立的群体，最可能由逐渐消退的恒星形成旋涡星系或经历并合的中到高质量旋涡星系形成。本样本中的SFS0s不能由本样本中接收下落气体的宁静S0星系形成，它们也不能消退以产生这些qS0s。
英文摘要
Lenticular (or S0) galaxies that remain actively star-forming (SFS0s) are a unique transition population among galaxies. We investigated the HI (21cm) neutral hydrogen content of a sample of lenticular galaxies identified from within the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey and which have been classified as star-forming or quiescent (qS0s). We compared these populations to each other and to a sample of star-forming spiral galaxies in MaNGA. We found that the HI Mass fraction and HI Deficiency of the SFS0s were intermediate between the quiescent S0s and the star-forming spirals, but most similar to the spirals. The HI depletion times of the quiescent S0's is very much longer than that of the SFS0 and spirals, which have roughly similar times. We also compared the molecular gas fractions of the three groups which shows that the lowest fraction of the three populations, followed by the star-forming S0s and then the star-forming spirals. A comparison of total baryonic mass comparisons indicates that the star-forming S0s have significantly lower masses than the qS0s in the sample. This suggests that the star-forming S0s must form from lower-mass progenitors (unobserved by MaNGA) which either accrete external gas, or loose spiral arms. The more massive quiescent S0s are a completely separate population, most likely to be formed either from fading star-forming spirals or from medium- to high-mass spirals undergoing mergers. The SFS0s in this sample cannot form from the quiescent S0s in this sample that receive in-falling gas, nor can they fade to create these qS0s.
发表机构
- Universiti Malaya（马来亚大学）
- Haverford College（哈弗福德学院）
- Space Telescope Science Institute（太空望远镜科学研究所）
- Johns Hopkins University（约翰斯·霍普金斯大学）
- National Centre for Particle Physics, Universiti Malaya（马来亚大学国家粒子物理中心）
机构由 AI 辅助整理，请以论文原文为准。
