The H i velocity function: a test of cosmology or baryon physics?

Chauhan, Garima; Lagos, Claudia del P.; Obreschkow, Danail; Power, Chris; Oman, Kyle A.; Elahi, Pascal J.

doi:10.1093/mnras/stz2069

Cited by 40 publications

(34 citation statements)

References 80 publications

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“…Recently, Lagos et al (2018) presented a new semi-analytic model of galaxy formation, S , with improvements over previous SAMs in the ability to reproduce galaxy scaling relations. Chauhan et al (2019) also recently showed that S is able to reproduce the HI mass-velocity width relation observed by the AL-FALFA survey. It is thus interesting to see if the tension between observations and simulations extends to the S implementation as well.…”

Section: Comparison With Semi-analytical Models Of Galaxy Formationmentioning

confidence: 80%

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

Catinella

Cortese

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use spectral stacking to measure the contribution of galaxies of different masses and in different hierarchies to the cosmic atomic hydrogen (HI) mass density in the local Universe. Our sample includes 1793 galaxies at z < 0.11 observed with the Westerbork Synthesis Radio Telescope, for which Sloan Digital Sky Survey spectroscopy and hierarchy information are also available. We find a cosmic HI mass density of Ω HI = (3.99 ± 0.54) × 10 −4 h −1 70 at z = 0.065. For the central and satellite galaxies, we obtain Ω HI of (3.51 ± 0.49) × 10 −4 h −1 70 and (0.90 ± 0.16) × 10 −4 h −1 70 , respectively. We show that galaxies above and below stellar masses of ∼10 9.3 M ⊙ contribute in roughly equal measure to the global value of Ω HI . While consistent with estimates based on targeted HI surveys, our results are in tension with previous theoretical work. We show that these differences are, at least partly, due to the empirical recipe used to set the partition between atomic and molecular hydrogen in semi-analytical models. Moreover, comparing our measurements with the cosmological semi-analytic models of galaxy formation S and GALFORM reveals gradual stripping of gas via ram pressure works better to fully reproduce the properties of satellite galaxies in our sample, than strangulation. Our findings highlight the power of this approach in constraining theoretical models, and confirm the non-negligible contribution of massive galaxies to the HI mass budget of the local Universe.At the same time, studies of the HI gas content of galax-

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Section: Comparison With Semi-analytical Models Of Galaxy Formationmentioning

confidence: 80%

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

Catinella

Cortese

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…This simulation relies on the 'Synthetic Uni-veRses For Surveys' (SURFS) simulations of cosmic structure (Elahi et al 2018), the SHARK semi-analytic model of galaxy evolution (Lagos et al 2018) and the STINGRAY mock sky builder (Obreschkow et al, in prep.). This threestep approach is conceptually identical to that of Chauhan et al (2019), used for the ALFALFA survey. To cover the full dynamic range of H I masses, the reference simulation concatenates two cubic simulation boxes with volumes of 40 3 h −1 Mpc (micro-SURFS) and 210 3 h −1 Mpc (medi-SURFS), respectively (where h = 0.6751).…”

Section: Survey Predictionsmentioning

confidence: 99%

WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

201

125

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The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (H I) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 × 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radioquiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (−90 • < δ < +30 • ) to a redshift of z 0.26, and generate spectral line image cubes at ∼30 arcsec resolution and ∼1.6 mJy beam −1 per 4 km s −1 channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect around half a million galaxies with a mean redshift of z ∼ 0.05 (∼200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the H I properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of recent and planned large-scale H I surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. -First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA).

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“…Mock H line profiles have also been used to reconcile the observed H velocity function with those obtained from cosmological simulations (e.g. Macciò et al 2016;Brooks et al 2017;Chauhan et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Drivers of asymmetry in synthetic H I emission-line profiles of galaxies in the EAGLE simulation

Manuwal,

Ludlow,

Stevens

et al. 2021

Preprint

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We study the shapes of spatially integrated H emission line profiles of galaxies in the simulation using three separate measures of the profile's asymmetry. We show that the subset of galaxies whose gas fractions and stellar masses are consistent with those in the xGASS survey also have similar H line asymmetries. Central galaxies with symmetric H line profiles typically correspond to rotationally supported H and stellar disks, but those with asymmetric line profiles may or may not correspond to dispersion-dominated systems. Galaxies with symmetric H emission lines are, on average, more gas rich than those with asymmetric lines, and also exhibit systematic differences in their specific star formation rates, suggesting that turbulence generated by stellar or AGN feedback may be one factor contributing to H line asymmetry. The line asymmetry also correlates strongly with the dynamical state of a galaxy's host dark matter halo: older, more relaxed haloes host more-symmetric galaxies than those hosted by unrelaxed ones. At fixed halo mass, asymmetric centrals tend to be surrounded by a larger number of massive subhaloes than their symmetric counterparts, and also experience higher rates of gas accretion and outflow. At fixed stellar mass, central galaxies have, on average, more symmetric H emission lines than satellites; for the latter, ram pressure and tidal stripping are significant sources of asymmetry.

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The H i velocity function: a test of cosmology or baryon physics?

Cited by 40 publications

References 80 publications

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

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

WALLABY – an SKA Pathfinder H i survey

Drivers of asymmetry in synthetic H I emission-line profiles of galaxies in the EAGLE simulation

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