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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

A tale of two galaxies: H i rich and poor in the star-forming J1051−17 galaxy group

  • V A Kilborn1,2
  • G Meurer3,4
  • R Džudžar1
  • S M Sweet1,2,5
  • K Bekki3,4
  • C Murugeshan1,2
  • A R H Stevens2,3
  • M Cluver1,2
  • T Jarrett1,6,7
7 affiliations
  1. 1Centre for Astrophysics and Supercomputing, Swinburne University of Technology , PO Box 218, Hawthorn, VIC 3122 ,
  2. 2ARC Centre of Excellence for All-Sky Astronomy (ASTRO3D)
  3. 3International Centre for Radio Astronomy Research (ICRAR) , M468
  4. 4The University of Western Australia , 35 Stirling Highway, Crawley, WA 6009 ,
  5. 5School of Mathematics and Physics, University of Queensland , Brisbane, QLD 4072 ,
  6. 6Institute for Astronomy, University of Hawaii , 2680 Woodlawn Drive, Honolulu, HI 96822 ,
  7. 7University of Cape Town Department of Astronomy, , Rondebosch, 7700 ,
Open at sourcePDFDOICite

Abstract

We report on multi-wavelength observations of the HIPASS J1051−17 galaxy group. Narrow-band Hα imaging revealed the original HIPASS H i source to be a galaxy group with at least 9 members, follow-up DEIMOS spectroscopy from Keck confirmed five new dwarf galaxies near the group, while six additional galaxies are confirmed by radial velocity matching in the surrounding field. We find no evidence of tidal dwarf galaxies in this group. One intriguing aspect of this galaxy group is the presence of two spiral galaxies in close proximity and of a similar stellar mass, but with vastly different H i masses. The H i-excess spiral is a polar ring galaxy with extended spiral arms, and the H i-deficient spiral is a more compact, high surface brightness galaxy with potentially up to ≈ 3 × higher star formation rate. The existence of two such spiral galaxies in the same environment shines a light on the internal processes governing galaxy formation, and highlights the importance of angular momentum on the star formation properties of galaxies. Such a detailed study illustrates the need to understand the physical processes in groups that give rise to the various scaling relations we observe.

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Cite

BibTeXRIS
BibTeX
@article{kilborn2026tale,
  title = {{A tale of two galaxies: H i rich and poor in the star-forming J1051−17 galaxy group}},
  author = {V A Kilborn and G Meurer and R Džudžar and S M Sweet and K Bekki and C Murugeshan and A R H Stevens and M Cluver and T Jarrett},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1879},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1879/8916636},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - A tale of two galaxies: H i rich and poor in the star-forming J1051−17 galaxy group
AU  - V A Kilborn
AU  - G Meurer
AU  - R Džudžar
AU  - S M Sweet
AU  - K Bekki
AU  - C Murugeshan
AU  - A R H Stevens
AU  - M Cluver
AU  - T Jarrett
PY  - 2026
DA  - 2026/10/14
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1879
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1879/8916636
AB  - We report on multi-wavelength observations of the HIPASS J1051−17 galaxy group. Narrow-band Hα imaging revealed the original HIPASS H i source to be a galaxy group with at least 9 members, follow-up DEIMOS spectroscopy from Keck confirmed five new dwarf galaxies near the group, while six additional galaxies are confirmed by radial velocity matching in the surrounding field. We find no evidence of tidal dwarf galaxies in this group. One intriguing aspect of this galaxy group is the presence of two spiral galaxies in close proximity and of a similar stellar mass, but with vastly different H i masses. The H i-excess spiral is a polar ring galaxy with extended spiral arms, and the H i-deficient spiral is a more compact, high surface brightness galaxy with potentially up to ≈ 3 × higher star formation rate. The existence of two such spiral galaxies in the same environment shines a light on the internal processes governing galaxy formation, and highlights the importance of angular momentum on the star formation properties of galaxies. Such a detailed study illustrates the need to understand the physical processes in groups that give rise to the various scaling relations we observe.
SN  - 0035-8711
SN  - 1365-2966
ER  -