The Neutral Hydrogen Gas Content of Star-forming and Quiescent S0 Galaxies

@misc{lee2026neutral,
  title = {{The Neutral Hydrogen Gas Content of Star-forming and Quiescent S0 Galaxies}},
  author = {D. A. A. Lee and Karen L. Masters and David V. Stark and Z. Z. Abidin},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2609.28030},
  eprint = {2609.28030},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.28030},
  note = {CC BY-SA 4.0},
}

TY  - UNPB
TI  - The Neutral Hydrogen Gas Content of Star-forming and Quiescent S0 Galaxies
AU  - D. A. A. Lee
AU  - Karen L. Masters
AU  - David V. Stark
AU  - Z. Z. Abidin
PY  - 2026
DA  - 2026/10/25
PB  - arXiv
DO  - 10.48550/arxiv.2609.28030
UR  - https://arxiv.org/abs/2609.28030
AB  - Lenticular (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 (SFSp) galaxies in MaNGA. We found that the HI mass fraction and HI deficiency of the SFS0s were intermediate between the qS0s and the SFSps, but more similar to the spirals. The HI depletion time of the qS0s is very much longer than that of the SFS0s 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 is found in the qS0s, followed by the SFS0s and then the SFSps. A comparison of total baryonic mass indicates that the SFS0s have significantly lower masses than the qS0s in the sample. This suggests that the SFS0s must form from lower mass progenitors (unobserved by MaNGA) which either accrete external gas or lose spiral arms. The more massive qS0s are a completely separate population, most likely to be formed either from fading SFSps or from medium- to high-mass spirals undergoing mergers. The SFS0s in this sample cannot form from the qS0s in this sample that receive in-falling gas, nor can they fade to create these qS0s.
ER  -