The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

Calette, A. R.; Ávila-Reese, V.; Rodríguez-Puebla, Aldo; Hernández-Toledo, H. M.; Papastergis, Emmanouil

doi:10.48550/arxiv.1803.07692

Cited by 10 publications

(11 citation statements)

References 107 publications

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“…Increasing the index reduces the star formation efficiency in low-mass halos and increases its efficiency in more massive halos and vice-versa for its reduction. Larger values of γ are in better agreement with the slope of the PL fit from Calette et al (2018), with γ ≥ 0.5 producing the closest match with their observational constraints. The robustness of the stellar mass to the power law dependence of the depletion time and even its normalization at the lower mass end in Figure A1 may point to the important role that t dep plays in setting the timescale for selfregulation to arise at high redshift.…”

Section: Discussionsupporting

confidence: 60%

“…Now we turn to the relation between the ISM gas and the stellar mass, which encodes star formation efficiency and can be constraining on models of galaxy evolution. Figure 4 compares the best-fit single power-law fit for the total cold gas mass as a function of M over the range 7.3 log (M /M halo ) 11.2 for late-type galaxies from Calette et al (2018) to the gas-to-stellar mass relation at z = 0 for the regulator model.…”

Section: Mism/m -M Relationmentioning

confidence: 99%

“…Figure4. Log of MISM/M from the regulator model as a function of stellar mass, compared to the best-fit single power-law fit for the total cold gas mass as a function of M over the range 7.3 log (M /M h ) 11.2 for late-type galaxies fromCalette et al (2018). Estimates of MISM/M are presented as a function of increasing the power-law dependence of wind mass-loading ηM (left), energy-loading ηE (middle), and metallicity-loading ηZ (right).…”

mentioning

confidence: 99%

“…Figure A2. Log of MISM/M from the regulator model as a function of stellar mass, compared to the best-fit single power-law fit for the total cold gas mass as a function of M over the range 7.3 log (M /M h ) 11.2 for late-type galaxies fromCalette et al (2018). Shaded lines correspond to alterations in the normalization of the depletion time C (left) and its power-law dependence with stellar mass, γ (right) and their respective influence on the MISM − M relation.…”

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confidence: 99%

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Regulation of Star Formation by a Hot Circumgalactic Medium

Carr¹,

Bryan²,

Fielding³

et al. 2022

Preprint

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Galactic outflows driven by supernovae (SNe) are thought to be a powerful regulator of a galaxy's star-forming efficiency. Mass, energy, and metal outflows (η M , η E , and η Z , here normalized by the star formation rate, the SNe energy and metal production rates, respectively) shape galaxy properties by both ejecting gas and metals out of the galaxy and by heating the circumgalactic medium (CGM), preventing future accretion. Traditionally, models have assumed that galaxies self-regulate by ejecting a large fraction of the gas which enters the interstellar medium (ISM), even though such high massloadings are in growing tension with observations. To better understand how the relative importance of ejective (i.e. high mass-loading) vs preventative (i.e. high energy-loading) feedback affects the present-day properties of galaxies, we develop a simple gas-regulator model of galaxy evolution, where the stellar mass, ISM, and CGM are modeled as distinct reservoirs which exchange mass, metals, and energy at different rates within a growing halo. Focusing on the halo mass range from 10 10 to 10 12 M , we demonstrate that, with reasonable parameter choices, we can reproduce the stellar-to-halo mass relation and the ISM-to-stellar mass relation with low mass-loaded (η M ∼ 0.1 − 10) but high energyloaded (η E ∼ 0.1 − 1) winds, with self-regulation occurring primarily through heating and cooling of the CGM. We show that the model predictions are robust against changes to the mass-loading of outflows but are quite sensitive to our choice of the energy-loading, preferring η E ∼ 1 for the lowest mass halos and ∼ 0.1 for Milky Way-like halos.

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Section: Discussionsupporting

confidence: 60%

Section: Mism/m -M Relationmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Regulation of Star Formation by a Hot Circumgalactic Medium

Carr¹,

Bryan²,

Fielding³

et al. 2022

Preprint

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“…late-type galaxies from Calette et al (2018) to the gas-to-stellar mass relation at z = 0 for the regulator model.…”

Section: Galaxy Scaling Relationsmentioning

confidence: 99%

Regulation of Star Formation by a Hot Circumgalactic Medium

Carr

Bryan

Fielding

et al. 2023

ApJ

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Galactic outflows driven by supernovae (SNe) are thought to be a powerful regulator of a galaxy’s star-forming efficiency. Mass, energy, and metal outflows (η M , η E , and η Z , here normalized by the star formation rate, the SNe energy, and metal production rates, respectively) shape galaxy properties by both ejecting gas and metals out of the galaxy and by heating the circumgalactic medium (CGM), preventing future accretion. Traditionally, models have assumed that galaxies self-regulate by ejecting a large fraction of the gas, which enters the interstellar medium (ISM), although whether such high mass loadings agree with observations is still unclear. To better understand how the relative importance of ejective (i.e., high mass loading) versus preventative (i.e., high energy loading) feedback affects the present-day properties of galaxies, we develop a simple gas-regulator model of galaxy evolution, where the stellar mass, ISM, and CGM are modeled as distinct reservoirs which exchange mass, metals, and energy at different rates within a growing halo. Focusing on the halo mass range from 1010 to 1012 M ⊙, we demonstrate that, with reasonable parameter choices, we can reproduce the stellar-to-halo mass relation and the ISM-to-stellar mass relation with low-mass-loaded (η M ∼ 0.1–10) but high-energy-loaded (η E ∼ 0.1–1) winds, with self-regulation occurring primarily through heating and cooling of the CGM. We show that the model predictions are robust against changes to the mass loading of outflows but are quite sensitive to our choice of the energy loading, preferring η E ∼ 1 for the lowest-mass halos and ∼0.1 for Milky Way–like halos.

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MIGHTEE-H i: the MH i – M* relation over the last billion years

Pan

Jarvis

Santos

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We study the MH i−M⋆ relation over the last billion years using the MIGHTEE-H i sample. We first model the upper envelope of the MH i−M⋆ relation with a Bayesian technique applied to a total number of 249 H i-selected galaxies, without binning the datasets, while taking account of the intrinsic scatter. We fit the envelope with both linear and non-linear models, and find that the non-linear model is preferred over the linear one with a measured transition stellar mass of log10(M⋆/M⊙) = 9.15 ± 0.87, beyond which the slope flattens. This finding supports the view that the lack of H i gas is ultimately responsible for the decreasing star formation rate observed in the massive main-sequence galaxies. For spirals alone, which are biased towards the massive galaxies in our sample, the slope beyond the transition mass is shallower than for the full sample, indicative of distinct gas processes ongoing for the spirals/high-mass galaxies from other types with lower stellar masses. We then create mock catalogues for the MIGHTEE-H i detections and non-detections with two main galaxy populations of late- and early-type galaxies to measure the underlying MH i−M⋆ relation. We find that the turnover in this relation persists whether considering the two galaxy populations as a whole or separately. We note that an underlying linear relation could mimic this turnover in the observed scaling relation, but a model with a turnover is strongly preferred. Measurements on the logarithmic average of H i masses against the stellar mass are provided as a benchmark for future studies.

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The $HI$- and $H_{2}$-to-stellar mass correlations of late- and early-type galaxies and their consistency with the observational mass functions

Cited by 10 publications

References 107 publications

Regulation of Star Formation by a Hot Circumgalactic Medium

Regulation of Star Formation by a Hot Circumgalactic Medium

Regulation of Star Formation by a Hot Circumgalactic Medium

MIGHTEE-H i: the MH i – M* relation over the last billion years

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