From massive spirals to dwarf irregulars: a new set of tight scaling relations for cold gas and stars driven by disc gravitational instability

Romeo, Alessandro

doi:10.1093/mnras/stz3367

Cited by 45 publications

(47 citation statements)

References 94 publications

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“…To match our relations, σ gas ∝ M ∼0.25 bar is required; however, it is observed that σ gas ∝ M 0.07 bar (e.g., Murugeshan et al 2020). Assuming a constantσ gas , as in Romeo (2020), this relation predicts j gas ∝ M bar at fixed f gas and j gas ∝ f gas at fixed M bar . Instead, a corollary of our gas relation is that j gas ∝ M 0.78 bar at fixed f gas and that j gas ∝ f 0.27 gas at fixed M bar .…”

Section: Disc Instabilitymentioning

confidence: 69%

“…Projecting our baryonic plane into the f gas − q diagram shows that galaxies of a given M bar follow parallel sequences of the form f gas ∝ q 1/β bar = q 2.22 , instead of f gas ∝ q 1.12 4 . Also based on disc instability, Romeo (2020) proposed a set of scaling relations of the form j iσi /(GM i ) ≈ 1, with i denoting stars or gas andσ a mass-weighted radial average of the velocity dispersion σ. This relation produces the scaling j * ∝ M 0.5 * (forσ * ∝ M 0.5 * , as proposed by Romeo 2020) and j gas ∝ M gas , very similar to the values found in MP21 for the 2D relations.…”

Section: Disc Instabilitymentioning

confidence: 99%

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A tight angular-momentum plane for disc galaxies

Piña

Posti

Pezzulli

et al. 2021

A&A

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The relations between the specific angular momenta (j) and masses (M) of galaxies are often used as a benchmark in analytic models and hydrodynamical simulations as they are considered to be amongst the most fundamental scaling relations. Using accurate measurements of the stellar (j*), gas (jgas), and baryonic (jbar) specific angular momenta for a large sample of disc galaxies, we report the discovery of tight correlations between j, M, and the cold gas fraction of the interstellar medium (fgas). At fixed fgas, galaxies follow parallel power laws in 2D (j, M) spaces, with gas-rich galaxies having a larger j* and jbar (but a lower jgas) than gas-poor ones. The slopes of the relations have a value around 0.7. These new relations are amongst the tightest known scaling laws for galaxies. In particular, the baryonic relation (jbar − Mbar − fgas), arguably the most fundamental of the three, is followed not only by typical discs but also by galaxies with extreme properties, such as size and gas content, and by galaxies previously claimed to be outliers of the standard 2D j − M relations. The stellar relation (j* − M* − fgas) may be connected to the known j* − M*-bulge fraction relation; however, we argue that the jbar − Mbar − fgas relation can originate from the radial variation in the star formation efficiency in galaxies, although it is not explained by current disc instability models.

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Section: Disc Instabilitymentioning

confidence: 69%

Section: Disc Instabilitymentioning

confidence: 99%

A tight angular-momentum plane for disc galaxies

Piña

Posti

Pezzulli

et al. 2021

A&A

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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%

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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“…The empirically based results presented here are optimal for comparing with these predictions as well as for calibrating theoretical models of galaxy evolution (see e.g. Romeo 2020). The results to be presented in this paper are the basis for further studies as the inference of the galaxy–halo connection extended to , , cold gas, and baryon masses.…”

Section: Introductionmentioning

confidence: 88%

The bivariate gas–stellar mass distributions and the mass functions of early- and late-type galaxies at

Rodríguez-Puebla

Calette

Ávila-Reese

et al. 2020

Publ. Astron. Soc. Aust.

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We report the bivariate $\rm HI$ - and $\rm H_{2}$ -stellar mass distributions of local galaxies in addition of an inventory of galaxy mass functions, MFs, for $\rm HI$ , $\rm H_{2}$ , cold gas, and baryonic mass, separately into early- and late-type galaxies. The MFs are determined using the $\rm HI$ and $\rm H_{2}$ conditional distributions and the galaxy stellar mass function (GSMF). For the conditional distributions we use the results from the compilation presented in Calette et al. [(2018) RMxAA, 54, 443.]. For determining the GSMF from $M_{*}\sim3\times10^{7}$ to $3\times10^{12}\ \text{M}_{\odot}$ , we combine two spectroscopic samples from the Sloan Digital Sky Survey at the redshift range $0.0033<z<0.2$ . We find that the low-mass end slope of the GSMF, after correcting from surface brightness incompleteness, is $\alpha\approx-1.4$ , consistent with previous determinations. The obtained $\rm HI\,$ MFs agree with radio blind surveys. Similarly, the $\rm H_{2}\,$ MFs are consistent with CO follow-up optically-selected samples. We estimate the impact of systematics due to mass-to-light ratios and find that our MFs are robust against systematic errors. We deconvolve our MFs from random errors to obtain the intrinsic MFs. Using the MFs, we calculate cosmic density parameters of all the baryonic components. Baryons locked inside galaxies represent 5.4% of the universal baryon content, while $\sim\! 96\%$ of the $\rm HI$ and $\rm H_{2}$ mass inside galaxies reside in late-type morphologies. Our results imply cosmic depletion times of $\rm H_{2}$ and total neutral H in late-type galaxies of $\sim\!1.3$ and 7.2 Gyr, respectively, which shows that late type galaxies are on average inefficient in converting $\rm H_{2}$ into stars and in transforming $\rm HI$ gas into $\rm H_{2}$ . Our results provide a fully self-consistent empirical description of galaxy demographics in terms of the bivariate gas–stellar mass distribution and their projections, the MFs. This description is ideal to compare and/or to constrain galaxy formation models.

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From massive spirals to dwarf irregulars: a new set of tight scaling relations for cold gas and stars driven by disc gravitational instability

Cited by 45 publications

References 94 publications

A tight angular-momentum plane for disc galaxies

A tight angular-momentum plane for disc galaxies

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

The bivariate gas–stellar mass distributions and the mass functions of early- and late-type galaxies at

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