Origin of the galaxy H i size–mass relation

Stevens, Adam; Diemer, Benedikt; Lagos, Claudia del P.; Nelson, Dylan; Obreschkow, Danail; Wang, Jing; Marinacci, Federico

doi:10.1093/mnras/stz2513

Cited by 50 publications

(56 citation statements)

References 92 publications

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“…On the other hand, the optically thin nature of the Hi emission leads to the possibility of probing possible gas inflows via the asymmetry of the line profile (Bournaud et al 2005;Deg et al 2020). The Hi fluxes are found to very closely follow scaling relations such as the star formation rate (SFR) surface density Σ SFR and the combined surface density of molecular (H 2 ) and Hi gas, Σ HI +H 2 (Schmidt 1959;Kennicutt 1998), Hi mass versus stellar mass (Huang et al 2012;Maddox et al 2015;Romeo 2020), Hi mass versus Hi size (Wang et al 2016;Stevens et al 2019), and the Hi-to-H 2 ratio as a function of stellar or gas surface density (Leroy et al 2008). These relations enable us to reveal important information even when we are unable to perform spatially resolved Hi observations (Giovanelli & Haynes 2015).…”

Section: Introductionmentioning

confidence: 78%

“…We can roughly estimate the dynamical mass based on the Hi FWHM, and Hi radius (R Hi ) by M Hi dyn = (FWHM/2/ sin θ) 2 R Hi /G, where θ is the Hi inclination angle and R Hi is the Hi radius. Since for galaxies the Hi size is tightly correlated with the Hi mass (Wang et al 2016;Stevens et al 2019), the R Hi can be estimated from M Hi using the relation derived by Wang et al (2016). For the Hi mass range of 9.5 < log(M Hi /M ) < 10, the Hi radius is in the range of 16.5 to 30 kpc (see Eq.…”

Section: Dynamical Massesmentioning

confidence: 99%

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The atomic gas of star-forming galaxies atz∼ 0.05 as revealed by the Five-hundred-meter Aperture Spherical Radio Telescope

Cheng

Ibar

Molina

et al. 2020

A&A

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Context. We report new H I observations of four z ∼ 0.05 VALES galaxies undertaken during the commissioning phase of the Five-hundred-meter Aperture Spherical Radio Telescope (FAST). Aims. FAST is the largest single-dish telescope in the world, with a 500 m aperture and a 19-Beam receiver. Exploiting the unprecedented sensitivity provided by FAST, we aim to study the atomic gas content, via the H I 21 cm emission line, in low-z star formation galaxies taken from the Valparaíso ALMA/APEX Line Emission Survey (VALES). Together with previous Atacama Large Millimeter/submillimeter Array (ALMA) CO(J = 1−0) observations, the H I data provides crucial information to measure the gas mass and dynamics. Methods. As a pilot H I galaxy survey, we targeted four local star-forming galaxies at z ∼ 0.05. In particular, one of them has already been detected in H I by the Arecibo Legacy Fast ALFA survey (ALFALFA), allowing a careful comparison. We use an ON-OFF observing approach that allowed us to reach an rms of 0.7 mJy beam−1 at a 1.7 km s−1 velocity resolution within only 20 min ON-target integration time. Results. In this Letter, we demonstrate the extraordinary capability of the FAST 19-beam receiver to push the detectability of the H I emission line of extra-galactic sources. The H I emission line detected by FAST shows good consistency with the previous Arecibo telescope ALFALFA results. Our observations are put into context with previous multi-wavelength data to reveal the physical properties of these low-z galaxies. We find that the CO(J = 1−0) and H I emission line profiles are similar. The dynamical mass estimated from the H I data is an order of magnitude higher than the baryon mass and the dynamical mass derived from the CO observations, implying that the mass probed by dynamics of H I is dominated by the dark matter halo. In one case, a target shows an excess of CO(J = 1−0) in the line centre, which can be explained by an enhanced CO(J = 1−0) emission induced by a nuclear starburst showing high-velocity dispersion.

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Section: Introductionmentioning

confidence: 78%

Section: Dynamical Massesmentioning

confidence: 99%

The atomic gas of star-forming galaxies atz∼ 0.05 as revealed by the Five-hundred-meter Aperture Spherical Radio Telescope

Cheng

Ibar

Molina

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…We can compare these radii to the observed H size-mass relation, R 1 = M HI /12.88 where R 1 in pc is the radius at which the surface density drops to 1 M pc −2 , and M HI is in solar masses (Stevens et al 2019b). This gives, for log M HI = [8, 9, 10, 11], 8, 8.8, 28, 88] kpc.…”

Section: Comparison Of Modelsmentioning

confidence: 99%

Galaxy cold gas contents in modern cosmological hydrodynamic simulations

Davé

Crain

Stevens

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

108

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Abstract We present a comparison of galaxy atomic and molecular gas properties in three recent cosmological hydrodynamic simulations, Simba, EAGLE, and IllustrisTNG, versus observations from z ∼ 0 − 2. These simulations all rely on similar sub-resolution prescriptions to model cold interstellar gas which they cannot represent directly, and qualitatively reproduce the observed z ≈ 0 H i and H2 mass functions (HIMF, H2MF), CO(1-0) luminosity functions (COLF), and gas scaling relations versus stellar mass, specific star formation rate, and stellar surface density μ*, with some quantitative differences. To compare to the COLF, we apply an H2-to-CO conversion factor to the simulated galaxies based on their average molecular surface density and metallicity, yielding substantial variations in αCO and significant differences between models. Using this, predicted z = 0 COLFs agree better with data than predicted H2MFs. Out to z ∼ 2, EAGLE’s and Simba’s HIMF and COLF strongly increase, while IllustrisTNG’s HIMF declines and COLF evolves slowly. EAGLE and Simba reproduce high LCO1-0 galaxies at z ∼ 1 − 2 as observed, owing partly to a median αCO(z = 2) ∼ 1 versus αCO(z = 0) ∼ 3. Examining H i, H2, and CO scaling relations, their trends with M* are broadly reproduced in all models, but EAGLE yields too little H i in green valley galaxies, IllustrisTNG and Simba overproduce cold gas in massive galaxies, and Simba overproduces molecular gas in small systems. Using Simba variants that exclude individual AGN feedback modules, we find that Simba’s AGN jet feedback is primarily responsible by lowering cold gas contents from z ∼ 1 → 0 by suppressing cold gas in $M_*\gtrsim10^{10}{\rm M}_\odot$ galaxies, while X-ray feedback suppresses the formation of high-μ* systems.

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“…b See also Stevens et al (2019b) for an extensive discussion on the origin of the small observed scatter of the HI mass versus HI size relation.…”

Section: Definitions Based On Colour and Structural Propertiesmentioning

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.

125

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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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Origin of the galaxy H i size–mass relation

Cited by 50 publications

References 92 publications

The atomic gas of star-forming galaxies atz∼ 0.05 as revealed by the Five-hundred-meter Aperture Spherical Radio Telescope

The atomic gas of star-forming galaxies atz∼ 0.05 as revealed by the Five-hundred-meter Aperture Spherical Radio Telescope

Galaxy cold gas contents in modern cosmological hydrodynamic simulations

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

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