The H i mass function of group galaxies in the ALFALFA survey

Jones, M. G. K.; Hess, Kelley M.; Adams, Elizabeth A. K.; Verdes–Montenegro, L.

doi:10.1093/mnras/staa810

Cited by 24 publications

(21 citation statements)

References 61 publications

(143 reference statements)

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“…We refer the readers to Guo et al (2020a) for more details. The measurements of Hi mass functions of this catalog have been presented in Jones et al (2020). As a result, our final sample consists of 22, 810 central galaxies in the Hi spectral stacking.…”

Section: Hi and Optical Samplesmentioning

confidence: 99%

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Guo,

Jones,

Wang

et al. 2021

Preprint

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We quantitatively investigate the dependence of central galaxy Hi mass (M HI ) on the stellar mass (M * ), halo mass (M h ), star formation rate (SFR), and central stellar surface density within 1 kpc (Σ 1 ), taking advantage of the Hi spectra stacking technique using both the Arecibo Fast Legacy ALFA Survey and the Sloan Digital Sky Survey. We find that the shapes of M HI -M h and M HI -M * relations are remarkably similar for both star-forming and quenched galaxies, with massive quenched galaxies having constantly lower Hi masses of around 0.6 dex. This similarity strongly suggests that neither halo mass nor stellar mass is the direct cause of quenching, but rather the depletion of Hi reservoir. While the Hi reservoir for low-mass galaxies of M * < 10 10.5 M strongly increases with M h , more massive galaxies show no significant dependence of M HI with M h , indicating the effect of halo to determine the smooth cold gas accretion. We find that the star formation and quenching of central galaxies are directly regulated by the available Hi reservoir, with an average relation of SFR ∝ M 2.75 HI /M 0.40 * , implying a quasi-steady state of star formation. We further confirm that galaxies are depleted of their Hi reservoir once they drop off the star-formation main sequence and there is a very tight and consistent correlation between M HI and Σ 1 in this phase, with M HI ∝ Σ −2 1 . This result is in consistent with the compaction-triggered quenching scenario, with galaxies going through three evolutionary phases of cold gas accretion, compaction and post-compaction, and quenching.

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Section: Hi and Optical Samplesmentioning

confidence: 99%

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Guo,

Jones,

Wang

et al. 2021

Preprint

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“…Furthermore, this consistency suggests that similar quenching processes typically invoked for dwarf galaxies in the Local Group are likely to be at play in these other systems. Similarly, more massive satellites have been shown to be quenched and/or gas-poor in accordingly higher density environments such as groups and clusters (Brown et al 2015(Brown et al , 2017Jones et al 2020), reaffirming the greater susceptibility of lower mass halos to environmental effects leading to their eventual quenching as seen in hydrodynamical simulations (Fillingham et While the observations presented in this work are an important step towards understanding the H properties of other satellites systems in the Local Volume, we briefly consider the parameter space that will be probed by upcoming H surveys. In Figure 5, we show log(𝑀 H ) as a function of log(𝐿 𝑉 ) for the Local Volume (stars and triangles) and Local Group (squares and circles) satellites coloured by their gas richness, log(𝑀 H /𝐿 𝑉 ).…”

Section: Discussion and Summarymentioning

confidence: 99%

HI Properties of Satellite Galaxies around Local Volume Hosts

Karunakaran,

Spekkens,

Carroll

et al. 2022

Preprint

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We present neutral atomic hydrogen (H ) observations using the Robert C. Byrd Green Bank Telescope (GBT) along the lines of sight to 49 dwarf satellite galaxy candidates around eight Local Volume systems (M104, M51, NGC1023, NGC1156, NGC2903, NGC4258, NGC4565, NGC4631). We detect the H reservoirs of two candidates (dw0934+2204 and dw1238−1122) and confirm them as background sources relative to their nearest foreground host systems. The remaining 47 satellite candidates are not detected in H , and we place stringent 5𝜎 upper limits on their H mass. We note that some (15/47) of our non-detections stem from satellites being occluded by their putative host's H emission. In addition to these new observations, we compile literature estimates on the H mass for an additional 17 satellites. We compare the H properties of these satellites to those within the Local Group, finding broad agreement between them. Crucially, these observations probe a "transition" region between −10 𝑀 𝑉 −14 where we see a mixture of gas-rich and gas-poor satellites and where quenching processes shift from longer timescales (i.e. via starvation) to shorter ones (i.e. via stripping). While there are many gas-poor satellites within this region, some are gas rich and suggests that the transition towards predominantly gas-rich satellites occurs at 𝐿 𝑉 ∼ 10 7 𝐿 , in line with simulations. The observations presented here are a key step toward characterizing the properties of dwarf satellite galaxies around Local Volume systems and future wide-field radio surveys with higher angular resolution (e.g. WALLABY) will vastly improve upon the study of such systems.

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“…H gas is the fundamental fuel for molecular gas and star formation and plays an essential role in galaxy formation and evolution and models thereof. Blind H surveys of the local Universe provide constraints on the H abundance via the H mass function (Jones et al 2020;Zwaan et al 2003) and the global H abundance Ω H = (4.3 ± 0.3)10 −4 ℎ 70 (Martin et al 2010). Spectral stacking techniques have also been used (see e.g.…”

Section: Introductionmentioning

confidence: 99%

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

Wolz,

Pourtsidou,

Masui

et al. 2021

Preprint

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We present the joint analysis of Neutral Hydrogen (H ) Intensity Mapping observations with three galaxy samples: the Luminous Red Galaxy (LRG) and Emission Line Galaxy (ELG) samples from the eBOSS survey, and the WiggleZ Dark Energy Survey sample. The H intensity maps are Green Bank Telescope observations of the redshifted 21cm emission on 100 deg 2 covering the redshift range 0.6 < 𝑧 < 1.0. We process the data by separating and removing the foregrounds present in the radio frequencies with F ICA. We verify the quality of the foreground separation with mock realisations, and construct a transfer function to correct for the effects of foreground removal on the H signal. We cross-correlate the cleaned H data with the galaxy samples and study the overall amplitude as well as the scale-dependence of the power spectrum. We also qualitatively compare our findings with the predictions by a semi-analytic galaxy evolution simulation. The cross-correlations constrain the quantity Ω H 𝑏 H 𝑟 H ,opt at an effective scale 𝑘 eff , where Ω H is the H density fraction, 𝑏 H is the H bias, and 𝑟 H ,opt the galaxyhydrogen correlation coefficient, which is dependent on the H content of the optical galaxy sample. At 𝑘 eff = 0.31 ℎ/Mpc we find Ω H 𝑏 H 𝑟 H ,Wig = [0.58 ± 0.09 (stat) ± 0.05 (sys)] × 10 −3 for GBT-WiggleZ, Ω H 𝑏 H 𝑟 H ,ELG = [0.40 ± 0.09 (stat) ± 0.04 (sys)] × 10 −3 for GBT-ELG, and Ω H 𝑏 H 𝑟 H ,LRG = [0.35 ± 0.08 (stat) ± 0.03 (sys)] × 10 −3 for GBT-LRG, at 𝑧 0.8. We also report results at 𝑘 eff = 0.24 ℎ/Mpc and 𝑘 eff = 0.48 ℎ/Mpc. With little information on H parameters beyond our local Universe, these are amongst the most precise constraints on neutral hydrogen density fluctuations in an underexplored redshift range.

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The H i mass function of group galaxies in the ALFALFA survey

Cited by 24 publications

References 61 publications

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

HI Properties of Satellite Galaxies around Local Volume Hosts

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

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