Dependence of Nebular Heavy-Element Abundance on H I Content for Spiral Galaxies

Robertson, Paul; Shields, G. A.; Davé, Romeel; Blanc, Guillermo A.; Wright, Audrey L.

doi:10.1088/0004-637x/773/1/4

Cited by 9 publications

(6 citation statements)

References 31 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…9, left panel). A similar anti-correlation between HI mass excess and metallicity has been found by Robertson et al (2013). Hughes et al (2013) also find the anti-correlation between metallicity and gas mass at fixed stellar mass in a volume-limited sample of 260 nearby late-type galaxies.…”

Section: The Stellar Mass-metallicity-sfr Relationshipsupporting

confidence: 79%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

View full text Add to dashboard Cite

Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

show abstract

Section: The Stellar Mass-metallicity-sfr Relationshipsupporting

confidence: 79%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

View full text Add to dashboard Cite

show abstract

“…9, left panel). A similar anti-correlation between HI mass excess and metallicity has been found by Robertson et al (2013). Hughes et al ( 2013) also find the anti-correlation between metallicity and gas mass at fixed stellar mass in a volumelimited sample of 260 nearby late-type galaxies.…”

Section: 2supporting

confidence: 73%

Star formation sustained by gas accretion

Almeida,

Elmegreen,

Munoz-Tunon

et al. 2014

Preprint

View full text Add to dashboard Cite

Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship between stellar mass, metallicity, and star formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

show abstract

“…Mufasa predicts a slope for ∆ log fHI vs. ∆ log Z of −0.18, similar to but slightly stronger than that vs. ∆ logsSFR. Robertson et al (2013) measured this deviation slope to be −0.41 ± 0.14 for field galaxies (−0.31 for cluster galaxies). This is steeper than our current predictions, but this was done at a fixed sSFR rather than M * , which likely accounts for some of the difference.…”

Section: Fluctuations Around Scaling Relationsmentioning

confidence: 96%

Mufasa: Galaxy star formation, gas, and metal properties across cosmic time

Davé

Rafieferantsoa

Thompson

et al. 2017

Mon. Not. R. Astron. Soc.

Self Cite

176

226

View full text Add to dashboard Cite

We examine galaxy star formation rates (SFRs), metallicities, and gas contents predicted by the Mufasa cosmological hydrodynamic simulations, which employ meshless hydrodynamics and novel feedback prescriptions that yield a good match to observed galaxy stellar mass assembly. We combine 50, 25, and 12.5h −1 Mpc boxes with a quarter billion particles each to show that Mufasa broadly reproduces a wide range of relevant observations, including SFR and specific SFR functions, the mass-metallicity relation, H i and H 2 fractions, H i (21 cm) and CO luminosity functions, and cosmic gas density evolution. There are mild but significant discrepancies, such as too many high-SFR galaxies, overly metal-rich and H i-poor galaxies at M * 10 10 M , and sS-FRs that are too low at z ∼ 1 − 2. The H i mass function increases by ×2 out to z ∼ 1 then steepens to higher redshifts, while the CO luminosity function computed using the Narayanan et al. conversion factor shows a rapid increase of CO-bright galaxies out to z ∼ 2 in accord with data. Ω HI and Ω H2 both scale roughly as ∝ (1 + z) 0.7 out to z ∼ 3, comparable to the rise in H i and H 2 fractions. Mufasa galaxies with high SFR at a given M * have lower metallicities and higher H i and H 2 fractions, following observed trends; we make quantitative predictions for how fluctuations in the baryon cycle drive correlated scatter around galaxy scaling relations. Most of these trends are well converged with numerical resolution. These successes highlight Mufasa as a viable platform to study many facets of cosmological galaxy evolution.

show abstract

Dependence of Nebular Heavy-Element Abundance on H I Content for Spiral Galaxies

Cited by 9 publications

References 31 publications

Star formation sustained by gas accretion

Star formation sustained by gas accretion

Star formation sustained by gas accretion

Mufasa: Galaxy star formation, gas, and metal properties across cosmic time

Contact Info

Product

Resources

About