Data

Data from: Angular momentum-related probe of cold gas deficiencies

The University of Western Australia
Li, Jie ; Obreschkow, Danail ; Lagos Urbina, Claudia ; Cortese, Luca ; Welker, Charlotte ; Džudžar, Robert
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ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2FANDS&rft_id=https://research-repository.uwa.edu.au/en/datasets/8b8734b0-bcd5-4231-9787-0efa0e83b443&rft.title=Data from: Angular momentum-related probe of cold gas deficiencies&rft.identifier=8b8734b0-bcd5-4231-9787-0efa0e83b443&rft.publisher=SAO/NASA Astrophysics Data System (ADS)&rft.description=Recent studies of neutral atomic hydrogen (H I) in nearby galaxies found that all field disc galaxies are H I saturated, in that they carry roughly as much H I as permitted before this gas becomes gravitationally unstable. By taking this H I saturation for granted, the atomic gas fraction fatm of galactic discs can be predicted as a function of the stability parameter q = jσ/(GM), where Mand jare the baryonic mass and specific angular momentum of the disc and σ is the H I velocity dispersion (Obreschkow et al. 2016). The log-ratio Δfq between this predictor and the observed atomic fraction can be seen as a physically motivated ‘H I deficiency’. While field disc galaxies have Δfq ≈ 0, objects subject to environmental removal of H I are expected to have Δfq > 0. Within this framework, we revisit the H I deficiencies of satellite galaxies in the Virgo cluster and in clusters of the EAGLE simulation. We find that observed and simulated cluster galaxies are H I deficient and that Δfq slightly increases when getting closer to the cluster centres. The Δfq values are similar to traditional H I deficiency estimators, but Δfq is more directly comparable between observations and simulations than morphology-based–deficiency estimators. By tracking the simulated H I deficient cluster galaxies back in time, we confirm that Δfq ≈ 0 until the galaxies first enter a halo with Mhalo > 1013M☉, at which moment they quickly lose H I by environmental effects. Finally, we use the simulation to investigate the links between Δfq and quenching of star formation.&rft.creator=Li, Jie &rft.creator=Obreschkow, Danail &rft.creator=Lagos Urbina, Claudia &rft.creator=Cortese, Luca &rft.creator=Welker, Charlotte &rft.creator=Džudžar, Robert &rft.date=2020&rft.relation=http://research-repository.uwa.edu.au/en/publications/95b271b8-5054-4954-840e-434fe4f295c8&rft_subject=galaxies: evolution&rft_subject=galaxies: formation&rft_subject=galaxies: fundamental parameters&rft_subject=galaxies: kinematics and dynamics&rft_subject=Astrophysics - Astrophysics of Galaxies&rft.type=dataset&rft.language=English Access the data

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Recent studies of neutral atomic hydrogen (H I) in nearby galaxies found that all field disc galaxies are H I saturated, in that they carry roughly as much H I as permitted before this gas becomes gravitationally unstable. By taking this H I saturation for granted, the atomic gas fraction fatm of galactic discs can be predicted as a function of the stability parameter q = jσ/(GM), where Mand jare the baryonic mass and specific angular momentum of the disc and σ is the H I velocity dispersion (Obreschkow et al. 2016). The log-ratio Δfq between this predictor and the observed atomic fraction can be seen as a physically motivated ‘H I deficiency’. While field disc galaxies have Δfq ≈ 0, objects subject to environmental removal of H I are expected to have Δfq > 0. Within this framework, we revisit the H I deficiencies of satellite galaxies in the Virgo cluster and in clusters of the EAGLE simulation. We find that observed and simulated cluster galaxies are H I deficient and that Δfq slightly increases when getting closer to the cluster centres. The Δfq values are similar to traditional H I deficiency estimators, but Δfq is more directly comparable between observations and simulations than morphology-based–deficiency estimators. By tracking the simulated H I deficient cluster galaxies back in time, we confirm that Δfq ≈ 0 until the galaxies first enter a halo with Mhalo > 1013M☉, at which moment they quickly lose H I by environmental effects. Finally, we use the simulation to investigate the links between Δfq and quenching of star formation.

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External Organisations
Centre for Astrophysics and Supercomputing
Associated Persons
Jie Li (Creator); Charlotte Welker (Creator)Robert Džudžar (Creator)

Issued: 2020-02

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  • global : 8b8734b0-bcd5-4231-9787-0efa0e83b443