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PreprintCC BY 4.0arXiv

Virgo Filaments VII: MeerKAT HI-imaging of the VirgoIII filament

  • M. Ramatsoku
  • G. Nagaraj
  • P. Jablonka
  • R. A. Finn
  • B. Vulcani
  • G. Rudnick
  • F. Combes
  • G. De Lucia
  • G. Castignani
  • D. Zaritsky
  • Y. Bahè
  • R. A. Koopmann
2 more authors
  • D. Zakharova
  • K. Conger
Open at sourcePDFDOICite

Abstract

We present MeerKAT HI observations of galaxies in the nearby Virgo III filament. At a median distance of ∼30 Mpc, the filament extends over ≈16 Mpc across ∼56 deg2. Our survey comprises 15 targeted MeerKAT pointings centred on HI deficient galaxies. Multi-resolution HI imaging at 8-90 arcsec with an rms of ∼0.3 mJy beam−1 reaches column densities of ∼4×1020 to ∼4×1018 atoms cm−2. This probes HI in galaxy discs at ∼1.2 kpc resolution and their outskirts at ∼13.5 kpc. We detect HI emission from 80 sources within the 500-3000 km/s range; most are optically detected galaxies, while 10 per cent lack confirmed counterparts. We also identify three HI clouds without optical counterparts near an interacting system, possibly displaced during the interaction. Galaxies in the filament lie below the field HI gas-fraction scaling relations at fixed stellar mass. Crucially, ∼40 per cent of galaxies not selected for HI deficiency fall more than 1σ below these relations, with an even greater fraction lying under the mean relation itself, indicating that the low HI gas fractions are widespread in the filament rather than confined to the pre-selected deficient population. Quantifying HI morphologies using an asymmetry parameter, we find a wide range of disturbances without a clear trend with projected distance to the filament spine or local density, suggesting a combination of local interactions and the filament itself. This paper presents the survey description, catalogue, and HI atlas enabling investigations of gas removal mechanisms in Virgo III galaxies.

Versions

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Cite

BibTeXRIS
BibTeX
@misc{ramatsoku2026virgo,
  title = {{Virgo Filaments VII: MeerKAT HI-imaging of the VirgoIII filament}},
  author = {M. Ramatsoku and G. Nagaraj and P. Jablonka and R. A. Finn and B. Vulcani and G. Rudnick and F. Combes and G. De Lucia and G. Castignani and D. Zaritsky and Y. Bahè and R. A. Koopmann and D. Zakharova and K. Conger},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.09253},
  eprint = {2609.09253},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.09253},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Virgo Filaments VII: MeerKAT HI-imaging of the VirgoIII filament
AU  - M. Ramatsoku
AU  - G. Nagaraj
AU  - P. Jablonka
AU  - R. A. Finn
AU  - B. Vulcani
AU  - G. Rudnick
AU  - F. Combes
AU  - G. De Lucia
AU  - G. Castignani
AU  - D. Zaritsky
AU  - Y. Bahè
AU  - R. A. Koopmann
AU  - D. Zakharova
AU  - K. Conger
PY  - 2026
DA  - 2026/09/08
PB  - arXiv
DO  - 10.48550/arxiv.2609.09253
UR  - https://arxiv.org/abs/2609.09253
AB  - We present MeerKAT HI observations of galaxies in the nearby Virgo III filament. At a median distance of ∼30 Mpc, the filament extends over ≈16 Mpc across ∼56 deg^2. Our survey comprises 15 targeted MeerKAT pointings centred on HI deficient galaxies. Multi-resolution HI imaging at 8-90 arcsec with an rms of ∼0.3 mJy beam^−1 reaches column densities of ∼4×10^20 to ∼4×10^18 atoms cm^−2. This probes HI in galaxy discs at ∼1.2 kpc resolution and their outskirts at ∼13.5 kpc. We detect HI emission from 80 sources within the 500-3000 km/s range; most are optically detected galaxies, while 10 per cent lack confirmed counterparts. We also identify three HI clouds without optical counterparts near an interacting system, possibly displaced during the interaction. Galaxies in the filament lie below the field HI gas-fraction scaling relations at fixed stellar mass. Crucially, ∼40 per cent of galaxies not selected for HI deficiency fall more than 1σ below these relations, with an even greater fraction lying under the mean relation itself, indicating that the low HI gas fractions are widespread in the filament rather than confined to the pre-selected deficient population. Quantifying HI morphologies using an asymmetry parameter, we find a wide range of disturbances without a clear trend with projected distance to the filament spine or local density, suggesting a combination of local interactions and the filament itself. This paper presents the survey description, catalogue, and HI atlas enabling investigations of gas removal mechanisms in Virgo III galaxies.
ER  -