The Resolve Survey Atomic Gas Census and Environmental Influences on Galaxy Gas Reservoirs

Stark, David V.; Kannappan, Sheila J.; Eckert, K.; Florez, Jonathan; Hall, Kirsten; Watson, Linda C.; Hoversten, E. A.; Burchett, Joseph N.; Guynn, David T.; Baker, Ashley; Moffett, Amanda J.; Berlind, Andreas A.; Norris, Mark A.; Haynes, Martha P.; Giovanelli, Riccardo; Leroy, Adam K.; Pisano, D. J.; Wei, Lisa H.; González, Roberto; Calderon, Victor

doi:10.3847/0004-637x/832/2/126

Cited by 46 publications

(50 citation statements)

References 144 publications

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“…The optical spectroscopic survey underway enhances redshift completeness over the SDSS for superior environment metrics and will in the future enable analysis of kinematics and metallicities. Importantly for the present work, 21 cm observations presented in Stark et al (2016) provide an unusually complete, adaptive sensitivity H I mass inventory for RESOLVE galaxies.…”

Section: The Resolve Surveymentioning

confidence: 77%

“…The H I mass inventory for RESOLVE is fully described in Stark et al (2016). That 21 cm data release is ∼94% complete overall (94% in RESOLVE-A, 95% in RESOLVE-B), counting all galaxies with detections with signal-to-noise ratio S/N>5 or upper limits stronger than 1.4M H I /M * ∼0.05-0.1.…”

Section: H I Massesmentioning

confidence: 99%

“…The H I masses and upper limits for RESOLVE come from the blind 21 cm ALFALFA survey (Haynes et al 2011) as well as new observations with the GBT and Arecibo telescopes. To increase the yield from the basic ALFALFA data products, Stark et al (2016) extracted 140 lower S/N detections and upper limits for RESOLVE galaxies within the ALFALFA grids. In addition, they acquired pointed observations with the GBT and Arecibo telescopes obtaining H I data for 290 galaxies in RESOLVE-A and 337 galaxies in RESOLVE-B, targeting those with either no H I measurements or weak upper limits from ALFALFA.…”

Section: H I Massesmentioning

confidence: 99%

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The Origin of Faint Tidal Features around Galaxies in the RESOLVE Survey

Hood

Kannappan

Stark

et al. 2018

ApJ

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We study tidal features around galaxies in the REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey. Our sample consists of 1048 RESOLVE galaxies that overlap with the DECam Legacy Survey, which reaches an r-band 3σ depth of ∼27.9 mag arcsec −2 for a 100 arcsec 2 feature. Images were masked, smoothed, and inspected for tidal features such as streams, shells, or tails/arms. We find tidal features in 17 ±2 % of our galaxies, setting a lower limit on the true frequency. The frequency of tidal features in the gas-poor (gas-to-stellar mass ratio <0.1) subsample is lower than in the gas-rich subsample (13 ±3 % versus 19 ±2 %). Within the gas-poor subsample, galaxies with tidal features have higher stellar and halo masses, ∼3× closer distances to nearest neighbors (in the same group), and possibly fewer group members at fixed halo mass than galaxies without tidal features, but similar specific star formation rates. These results suggest tidal features in gas-poor galaxies are typically streams/shells from dry mergers or satellite disruption. In contrast, the presence of tidal features around gas-rich galaxies does not correlate with stellar or halo mass, suggesting these tidal features are often tails/arms from resonant interactions. Similar to tidal features in gas-poor galaxies, tidal features in gas-rich galaxies imply 1.7× closer nearest neighbors in the same group; however, they are associated with diskier morphologies, higher star formation rates, and higher gas content. In addition to interactions with known neighbors, we suggest that tidal features in gas-rich galaxies may arise from accretion of cosmic gas and/or gas-rich satellites below the survey limit.

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Section: The Resolve Surveymentioning

confidence: 77%

Section: H I Massesmentioning

confidence: 99%

Section: H I Massesmentioning

confidence: 99%

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The Origin of Faint Tidal Features around Galaxies in the RESOLVE Survey

Hood

Kannappan

Stark

et al. 2018

ApJ

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“…In addition it has nearly complete coverage by the GALEX MIS depth survey (∼ 1500s) in the NUV (Morrissey et al 2007), plus Swift uvm2 imaging for 19 galaxies (E15). The RESOLVE HI survey, presented in Stark et al (2016), provides unconfused (or deconfused) HI detections or strong upper limits (1.4M HI < 0.05M star ) for 87% of galaxies brighter than M r,tot = −17.0 or having estimated M cold bary > 10 9.0 M ⊙ , based on calibrations of the relationship between gas-to-stellar mass ratio and galaxy color (the photometric gas fractions technique described in E15).…”

Section: Data Setsmentioning

confidence: 99%

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Eckert

Kannappan

Lagos

et al. 2017

ApJ

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We examine the z = 0 group-integrated stellar and cold baryonic (stars + cold atomic gas) mass functions (group SMF and CBMF) and the baryonic collapse efficiency (group cold baryonic to dark matter halo mass ratio) using the RESOLVE and ECO survey galaxy group catalogs and a galform semi-analytic model (SAM) mock catalog. The group SMF and CBMF fall off more steeply at high masses and rise with a shallower low-mass slope than the theoretical halo mass function (HMF). The transition occurs at group-integrated cold baryonic mass M cold bary ∼ 10 11 M ⊙ . The SAM, however, has significantly fewer groups at the transition mass ∼1011 M ⊙ and a steeper low-mass slope than the data, suggesting that feedback is too weak in low-mass halos and conversely too strong near the transition mass. Using literature prescriptions to include hot halo gas and potential unobservable galaxy gas produces a group BMF with slope similar to the HMF even below the transition mass. Its normalization is lower by a factor of ∼2, in agreement with estimates of warm-hot gas making up the remaining difference. We compute baryonic collapse efficiency with the halo mass calculated two ways, via halo abundance matching (HAM) and via dynamics (extended all the way to three-galaxy groups using stacking). Using HAM, we find that baryonic collapse efficiencies reach a flat maximum for groups across the halo mass range of M halo ∼ 10 11.4−12 M ⊙ , which we label "nascent groups." Using dynamics, however, we find greater scatter in baryonic collapse efficiencies, likely indicating variation in group hot-to-cold baryon ratios. Similarly, we see higher scatter in baryonic collapse efficiencies in the SAM when using its true groups and their group halo masses as opposed to friends-of-friends groups and HAM masses.

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“…However, rather than a continuous trend of H i depletion as a function of environment (e.g. Stark et al 2016;Brown et al 2017), their work finds the role of environment to be more binary, determining whether or not galaxies have any H i at all. Higher-resolution runs of these simulations have found the H i fractions to increase Marasco et al 2016;Crain et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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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The Resolve Survey Atomic Gas Census and Environmental Influences on Galaxy Gas Reservoirs

Cited by 46 publications

References 144 publications

The Origin of Faint Tidal Features around Galaxies in the RESOLVE Survey

The Origin of Faint Tidal Features around Galaxies in the RESOLVE Survey

The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

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

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