Erratum: “Vla Imaging of Virgo Spirals in Atomic Gas (Viva). I. The Atlas and the H I Properties” (2009, Aj, 138, 1741)

Chung, Aeree; Gorkom, J. H. van; Kenney, Jeffrey D. P.; Crowl, Hugh H.; Vollmer, B.

doi:10.1088/0004-6256/139/6/2716

Cited by 311 publications

(692 citation statements)

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“…Recently a new VLA H I imaging survey of selected galaxies in the Virgo cluster (VIVA, VLA Imaging of Virgo spirals in Atomic gas) has been completed Chung et al 2009. This survey confirmed some already well known facts, e.g.…”

Section: The Other Extreme the Center Of Virgosupporting

confidence: 72%

H I Imaging Surveys: Gas and Galaxy Evolution in Different Environments

Gorkom

2010

Proc. IAU

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Abstract. Our understanding of the formation and evolution of galaxies and the large scale structure has advanced enormously over the last decade, thanks to an impressive synergy between theoretical and observational efforts. While the growth of the dark matter component seems well understood, the physics of the gas, during its accretion, removal and/or depletion is less well understood. Increasingly large scale optical surveys are tracing out the cosmic web of filaments and voids and mathematical tools have been developed to describe these structures and identify galaxies in specific environments. H I imaging surveys begin to answer the question: how do galaxies get and lose their gas. The best evidence for ongoing gas accretion is found in the lowest density environments, while removal of gas in the highest density environments stops star formation and reddens the galaxies. Although current H I emission surveys are limited to redshifts less than 0.2, this is where the LSS is best defined and much can be learned in the local universe.

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Section: The Other Extreme the Center Of Virgosupporting

confidence: 72%

H I Imaging Surveys: Gas and Galaxy Evolution in Different Environments

Gorkom

2010

Proc. IAU

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“…The spiral galaxies in the Ursa Major cluster do not show any prominent hint of HI deficiency or gas stripping (see Fig. 1 of Verheijen 2004), while many examples for ram pressure stripping are found in the Virgo cluster (e.g., Chung et al 2009). This is also supported by no detection of intracluster medium in the Ursa Major cluster (Verheijen & Sancisi 2001).…”

Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using SDSS-DR7 and NASA/IPAC Extragalactic Database spectroscopic data, we identify 166 galaxies as members of the Ursa Major cluster with M r < −13.5 mag. We morphological classify all galaxies by means of carefully inspecting g−, r−, i−band colour and monochromatic images. We show that the Ursa Major cluster is dominated by late-type galaxies, but also contains a significant number of earlytype galaxies, particularly in the dwarf regime. We present further evidence for the existence of several subgroups in the cluster, consistent with previous findings. The early-type fraction is found to correlate with the mass of the subgroup. We also investigate environmental effects by comparing the properties of the Ursa Major early-type dwarf galaxies to those of the Virgo cluster. In contrast to the Virgo, the red sequence of the Ursa Major cluster is only sparsely populated in the optical and ultraviolet colour-magnitude relations. It also shows a statistically significant gap between −18 < M r < −17 mag, i.e. the Ursa Major cluster lacks early-type dwarf galaxies at the bright end of their luminosity function. We discover that the majority of early-type dwarf galaxies in the Ursa Major cluster have blue cores with hints of recent or ongoing star formation. We suggest that gravitational tidal interactions can trigger central blue star forming regions in early-type dwarfs. After that, star formation would only fade completely when the galaxies experience ram pressure stripping or harassment, both of which are nearly absent in the Ursa Major cluster.

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“…This was exemplified in exquisite detail by the VLA 1 Imaging of Virgo in Atomic gas survey (VIVA; Chung et al 2009), which demonstrated the importance of the highest density environments in shutting down star formation via strong gas depletion mechanisms. Other observational (e.g.…”

Section: Introductionmentioning

confidence: 98%

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

Stevens

Brown

2017

Monthly Notices of the Royal Astronomical Society

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We combine the latest spectrally stacked data of 21-cm emission from the ALFALFA survey with an updated version of the Dark Sage semi-analytic model to investigate the relative contributions of secular and environmental astrophysical processes on shaping the H i fractions and quiescence of galaxies in the local Universe. We calibrate the model to match the observed mean H i fraction of all galaxies as a function of stellar mass. Without consideration of stellar feedback, disc instabilities, and active galactic nuclei, we show how the slope and normalisation of this relation would change significantly. We find Dark Sage can reproduce the relative impact that halo mass is observed to have on satellites' H i fractions and quiescent fraction. However, the model satellites are systematically gas-poor. We discuss how this could be affected by satellite-central cross-contamination from the group-finding algorithm applied to the observed galaxies, but that it is not the full story. From our results, we suggest the anti-correlation between satellites' H i fractions and host halo mass, seen at fixed stellar mass and fixed specific star formation rate, can be attributed almost entirely to ram-pressure stripping of cold gas. Meanwhile, stripping of hot gas from around the satellites drives the correlation of quiescent fraction with halo mass at fixed stellar mass. Further detail in the modelling of galaxy discs' centres is required to solidify this result, however. We contextualise our results with those from other semi-analytic models and hydrodynamic simulations.

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Erratum: “Vla Imaging of Virgo Spirals in Atomic Gas (Viva). I. The Atlas and the H I Properties” (2009, Aj, 138, 1741)

Abstract: Galaxy

Cited by 311 publications

References 0 publications

H I Imaging Surveys: Gas and Galaxy Evolution in Different Environments

H I Imaging Surveys: Gas and Galaxy Evolution in Different Environments

The properties of early-type galaxies in the Ursa Major cluster

Physical drivers of galaxies’ cold-gas content: exploring environmental and evolutionary effects with Dark Sage

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