The Inflow and Outflow Rate Evolution of Local Milky Way–mass Star-forming Galaxies since z = 1.3

Pan, Zhifen; Peng, Yingjie; Zheng, Xianzhong; Wang, Jing; Kong, Xu

doi:10.3847/1538-4357/ab11c2

Cited by 4 publications

(2 citation statements)

References 105 publications

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“…In this work, M H2 is derived by utilizing the scaling relation of Tacconi et al (2018). On the other hand, f is calculated using the M star − M HI relation of Pan et al (2019), assuming that this relation does not evolve during z = [0, 3]. As such, in each redshift bin, f can be determined by where M HI at ∆MS = 0 is from equation (4) of Pan et al (2019).…”

Section: Methodsmentioning

confidence: 99%

“…On the other hand, f is calculated using the M star − M HI relation of Pan et al (2019), assuming that this relation does not evolve during z = [0, 3]. As such, in each redshift bin, f can be determined by where M HI at ∆MS = 0 is from equation (4) of Pan et al (2019). We divide galaxies with a mass bin of ∆logM star = 0.1 dex and use the Monte Carlo method to derive the M baryon distribution of galaxies in each bin.…”

Section: Methodsmentioning

confidence: 99%

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The Evolution of Baryonic Mass Function of Galaxies to z = 3

Pan

Peng

Zheng

et al. 2019

ApJL

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We combine the published stellar mass function (SMF) and gas scaling relations to explore the baryonic (stellar plus cold gas) mass function (BMF) of galaxies to redshift z = 3. We find evidence that at log(M baryon /M ⊙ ) > 11.3, the BMF evolves little since z ∼ 2.2. With the evolution of BMF and SMF, we investigate the baryon net accretion rate (ρ baryon ) and stellar mass growth rate (ρ star ) for the galaxy population of log(M star /M ⊙ )>10. The ratio between these two quanties,ρ baryon /ρ star , decreases fromρ baryon /ρ star ∼2 at z ∼ 2.5 toρ baryon /ρ star <0.5 at z ∼ 0.5, suggesting that massive galaxies are transforming from the "accretion dominated" phase to the "depletion dominated" phase from high−z to low−z. The transition of these two phases occurs at z ∼ 1.5, which is consistent with the onset redshift of the decline of cosmic star formation rate density. This provides evidence to support the idea that the decline of cosmic star formation rate density since z ∼ 1.5 is mainly resulted from the decline of baryon net accretion rate and star formation quenching in galaxies.

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

The Evolution of Baryonic Mass Function of Galaxies to z = 3

Pan

Peng

Zheng

et al. 2019

ApJL

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Star formation histories of dwarf and giant galaxies with different supernovae-driven outflows: NGC 2403, NGC 628

Chattopadhyay

Ray

2023

New Astronomy

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The growth history of local M 33-mass bulgeless spiral galaxies

Kang,

Kudritzki,

Zhang

2023

A&A

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NGC 7793, NGC 300, M 33, and NGC 2403 are four nearby undisturbed and bulgeless low-mass spiral galaxies whose morphology and stellar mass are similar. They are ideal laboratories for studying disc formation scenarios and the histories of stellar mass growth. We constructed a simple chemical evolution model by assuming that discs grow gradually with continuous metal-free gas infall and metal-enriched gas outflow. By means of the classical χ2 method, applied to the model predictions, the best combination of free parameters capable of reproducing the corresponding present-day observations was determined, that is, the radial dependence of the infall timescale τ = 0.1r/Rd + 3.4 Gyr (Rd is the disc scale length) and the gas outflow efficiency bout = 0.2. The model results agree excellently with the general predictions of the inside-out growth scenario for the evolution of spiral galaxies. About 80% of the stellar mass of NGC 7793 was assembled within the last 8 Gyr, and 40% of the mass was assembled within the last 4 Gyr. By comparing the best-fitting model results of the three other galaxies, we obtain similar results: 72% (NGC 300), 66% (NGC 2403), and 79% (M 33) of the stellar mass were assembled within the last ∼8 Gyr (i.e. z = 1). These four disc galaxies simultaneously increased their sizes and stellar masses in time, and they grew in size at ∼0.30 times the rate at which they grew in mass. The scale lengths of these four discs now are 20%–25% larger than at z = 1. Our best-fitting model predicted the stellar mass-metallicity relation and the metallicity gradients, constrained by the observed metallicities from HII-region emission line analysis, agree well with the observations measured from individual massive red and blue supergiant stars and population synthesis of Sloan Digital Sky Survey galaxies.

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The Inflow and Outflow Rate Evolution of Local Milky Way–mass Star-forming Galaxies since z = 1.3

Cited by 4 publications

References 105 publications

The Evolution of Baryonic Mass Function of Galaxies to z = 3

The Evolution of Baryonic Mass Function of Galaxies to z = 3

Star formation histories of dwarf and giant galaxies with different supernovae-driven outflows: NGC 2403, NGC 628

The growth history of local M 33-mass bulgeless spiral galaxies

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