Nora SalemHaverford College, Karen MastersHaverford College, David StarkSTScI, Anubhav SharmaHaverford College
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引用次数: 0
Abstract
HI-rich galaxies typically have high star-formation rates (SFR), but there
exist interesting HI-rich and low star-forming (low-SF) galaxies. Previous work
on a sample of these galaxies identified from HI-MaNGA (HI follow-up to the
MaNGA survey) using an infrared indicator of specific-SFR (sSFR; namely
W2-W3~<2) could find no single physical process to explain their unusual
behaviour. The method by which galaxies are identified as low sSFR may be
important in this conclusion. In this Research Note, we explore how an HI-rich,
low sSFR sample of HI-MaNGA galaxies differs using H alpha, single stellar
population, and ultraviolet estimators of SFR. We find that samples are
statistically similar to each other so long as W2-W3~<2 is interpreted as
corresponding to sSFR<10^{-11.15} yr^{-1}.
富含 HI 的星系通常具有较高的恒星形成率（SFR），但也存在一些有趣的富含 HI 但恒星形成率较低（low-SF）的星系。以前的研究利用红外比SFR（即W2-W3~<2）指标，对从HI-MaNGA（MaNGA巡天的HI后续）中确定的这些星系样本进行了研究，但没有发现任何单一的物理过程可以解释它们的异常行为。在得出这一结论时，确定星系为低比SFR的方法可能很重要。在这份研究报告中，我们使用Hα、单恒星群和紫外线估计SFR的方法，探讨了富含HI、低sSFR的HI-MaNGA星系样本的不同之处。我们发现，只要将W2-W3~<2解释为对应于sSFR<10^{-11.15} yr^{-1}，样本之间在统计上是相似的。
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