The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

Hu, Wenkai; Catinella, Barbara; Cortese, Luca; Lagos, Claudia del P.; Chauhan, Garima; Oosterloo, Tom; Chen, Xuelei

doi:10.1093/mnras/staa257

Cited by 16 publications

(20 citation statements)

References 78 publications

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“…We compare the optical size, total stellar mass (M * ), specific angular momentum (via the q parameter), and (NUV-r)+μ *based approaches for galaxies with stellar masses between 10 9 and 10 11 M . The first three definitions are calibrated on central galaxies within 1.5σ from the SHARK main sequence of star-forming c Indeed, while SHARK shows improvements over previous semi-analytical models in reproducing galaxy scaling relations, there are still clear limitations when it comes to matching the gas properties of galaxies across environments (e.g., Hu et al 2020).…”

Section: A Direct Comparison Of Different Gas Deficiency Definitionsmentioning

confidence: 99%

“…By binning galaxies according to a given property (e.g., stellar mass, colour, morphology, etc.) and stacking the corresponding HI spectra in each bin, it is possible to study gas scaling relations (e.g., Fabello et al 2011Fabello et al , 2012Geréb, Morganti, & Oosterloo 2014;Brown et al 2015Brown et al , 2017Healy et al 2019;Guo et al 2020;Hu et al 2020).…”

Section: Hi Stripping In Groupsmentioning

confidence: 99%

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The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Cortese

Catinella

Smith

2021

Publ. Astron. Soc. Aust.

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124

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One of the key open questions in extragalactic astronomy is what stops star formation in galaxies. While it is clear that the cold gas reservoir, which fuels the formation of new stars, must be affected first, how this happens and what are the dominant physical mechanisms involved is still a matter of debate. At least for satellite galaxies, it is generally accepted that internal processes alone cannot be responsible for fully quenching their star formation, but that environment should play an important, if not dominant, role. In nearby clusters, we see examples of cold gas being removed from the star-forming discs of galaxies moving through the intracluster medium, but whether active stripping is widespread and/or necessary to halt star formation in satellites, or quenching is just a consequence of the inability of these galaxies to replenish their cold gas reservoirs, remains unclear. In this work, we review the current status of environmental studies of cold gas in star-forming satellites in the local Universe from an observational perspective, focusing on the evidence for a physical link between cold gas stripping and quenching of the star formation. We find that stripping of cold gas is ubiquitous in satellite galaxies in both group and cluster environments. While hydrodynamical mechanisms such as ram pressure are important, the emerging picture across the full range of dark matter halos and stellar masses is a complex one, where different physical mechanisms may act simultaneously and cannot always be easily separated. Most importantly, we show that stripping does not always lead to full quenching, as only a fraction of the cold gas reservoir might be affected at the first pericentre passage. We argue that this is a key point to reconcile apparent tensions between statistical and detailed analyses of satellite galaxies, as well as disagreements between various estimates of quenching timescales. We conclude by highlighting several outstanding questions where we expect to see substantial progress in the coming decades, thanks to the advent of the Square Kilometre Array and its precursors, as well as the next-generation optical and millimeter facilities.

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Section: A Direct Comparison Of Different Gas Deficiency Definitionsmentioning

confidence: 99%

Section: Hi Stripping In Groupsmentioning

confidence: 99%

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Cortese

Catinella

Smith

2021

Publ. Astron. Soc. Aust.

Self Cite

124

View full text Add to dashboard Cite

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“…In this work, we use a stacking method to explore how the H content and the specific star formation rate (sSFR) change with the group-centric radius. In Hu et al (2019, hereafter Paper I) and Hu et al (2020a), we have developed an interferometric stacking technique to measure the H content in galaxies and confirm that there is little evolution in cosmic H density (Ω H ) at low redshift ( < 0.11). This paper uses the same sample and technique to study the relation between H content and group-centric radius.…”

Section: Introductionmentioning

confidence: 72%

“…Following what done in Hu et al (2020a), we compare our results with the prediction from the S (Lagos et al 2018) semi-analytic model. We construct a lightcone with an area of ∼ 6900deg 2 and redshift range of = 0 − 0.1, containing all the galaxies with ★ ≥ 10 5 ⊙ (see Chauhan et al 2019 for details on how lightcones are constructed).…”

Section: Discussionmentioning

confidence: 89%

“…Directly removing confused galaxies will have the effect of removing massive centrals and gas-rich satellites. To correct for the effects of confusion in these galaxies without introducing bias, we follow the method in Fabello et al (2012) and Hu et al (2020a), where the total signal is estimated as the sum of the signal of the sample galaxy ( ) and the signal of the companions ( ) weighted with two overlap factors:…”

Section: Confusion Correctionmentioning

confidence: 99%

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The atomic hydrogen content of galaxies as a function of group-centric radius

Cortese

Catinella

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We apply a spectral stacking technique to Westerbork Synthesis Radio Telescope observations to measure the neutral atomic hydrogen content (H i) of nearby galaxies in and around galaxy groups at z < 0.11. Our sample includes 577 optically-selected galaxies (120 isolated galaxies and 457 satellites) covering stellar masses between 1010 and 1011.5 M⊙, cross-matched with Yang’s group catalogue, with angular and redshift positions from the Sloan Digital Sky Survey. We find that the satellites in the centres of groups have lower H i masses at fixed stellar mass and morphology (characterised by the inverse concentration index) relative to those at larger radii. These trends persist for satellites in both high-mass (Mhalo > 1013.5 h−1 M⊙) and low-mass (Mhalo ≤ 1013.5 h−1 M⊙) groups, but disappear if we only consider group members in low local density (Σ < 5 gal/Mpc−2) environments. Similar trends are found for the specific star formation rate. Interestingly, we find that the radial trends of decreasing H i mass with decreasing group-centric radius extend beyond the group virial radius, as isolated galaxies close to larger groups lack H i compared with those located more than ∼3.0 R180 away from the center of their nearest group. We also measure these trends in the late-type subsample and obtain similar results. Our results suggest that the H i reservoir of galaxies can be affected before galaxies become group satellites, indicating the existence of pre-processing in the infalling isolated galaxies.

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From rest-frame luminosity functions to observer-frame colour distributions: tackling the next challenge in cosmological simulations

Bravo

Lagos

Robotham

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abstract Galaxy spectral energy distributions (SEDs) remain among the most challenging yet informative quantities to reproduce in simulations due to the large and complex mixture of physical processes that shape the radiation output of a galaxy. With the increasing number of surveys utilising broadband colours as part of their target selection criteria, the production of realistic SEDs in simulations is necessary for assisting in survey design and interpretation of observations. The recent success in reproducing the observed luminosity functions (LF) from far-UV to far-IR, using the state-of-the-art semi-analytic model Shark and the SED generator ProSpect, represents a critical step towards better galaxy colour predictions. We show that with Shark and ProSpect we can closely reproduce the optical colour distributions observed in the panchromatic GAMA survey. The treatment of feedback, star formation, central-satellite interactions and radiation re-processing by dust are critical for this achievement. The first three processes create a bimodal distribution, while dust attenuation defines the location and shape of the blue and red populations. While a naive comparison between observation and simulations displays the known issue of over-quenching of satellite galaxies, the introduction of empirically-motivated observational errors and classification from the same group finder used in GAMA greatly reduces this tension. The introduction of random re-assignment of $\sim 15\%$ of centrals/satellites as satellites/centrals on the simulation classification closely resembles the outcome of the group finder, providing a computationally less intensive method to compare simulations with observations.

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The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

Cited by 16 publications

References 78 publications

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

The atomic hydrogen content of galaxies as a function of group-centric radius

From rest-frame luminosity functions to observer-frame colour distributions: tackling the next challenge in cosmological simulations

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