Redshift evolution of stellar mass versus gas fraction relation in 0 &lt;<i>z</i>&lt; 2 regime: observational constraint for galaxy formation models

Morokuma-Matsui, Kana; Baba, Junichi

doi:10.1093/mnras/stv2227

Cited by 21 publications

(14 citation statements)

References 157 publications

(263 reference statements)

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“…Our treatment of trends of FPZ parameters with z and M * as simple power laws is also highly over-simplified. As found by Lagos et al (2011Lagos et al ( , 2014; Morokuma-Matsui & Baba (2015), the redshift and M * dependence of gas-mass fractions is more complicated than this, as there are inflections and slight curvatures in the behavior of both quantities. Thus, our models are almost certainly not exact, but rather a simplified scaling aimed at a general representation of the trends necessary to explain the coevolution of SFR and metallicity.…”

Section: Redshift Variation Of the Stellar Mass Scalingmentioning

confidence: 83%

Coevolution of metallicity and star formation in galaxies toz≃ 3.7 – II. A theoretical model

Hunt

Dayal

Magrini

et al. 2016

Mon. Not. R. Astron. Soc.

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Recent work suggests that galaxy evolution, and the build-up of stellar mass (M * ) over cosmic time, is characterized by changes with redshift of star formation rate (SFR) and oxygen abundance (O/H). In a companion paper, we have compiled a large dataset to study Metallicity Evolution and Galaxy Assembly (MEGA), consisting of ∼1000 galaxies to z 3.7 with a common O/H calibration. Here we interpret the MEGA scaling relations of M * , SFR, and O/H with an updated version of the model presented by Dayal et al. (2013). This model successfully reproduces the observed O/H ratio of ∼80 000 galaxies selected from the Sloan Digital Sky Survey to within 0.05−0.06 dex. By extending the model to the higher redshift MEGA sample, we find that although the specific mass loading of outflows does not change measurably during the evolution, the accretion rate and gas content of galaxies increase significantly with redshift. These two effects can explain, either separately or possibly in tandem, the observed lower metal abundance of high-z galaxies.

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Section: Redshift Variation Of the Stellar Mass Scalingmentioning

confidence: 83%

Coevolution of metallicity and star formation in galaxies toz≃ 3.7 – II. A theoretical model

Hunt

Dayal

Magrini

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The tension in the comparison of the fraction of obscured star formation to dust-to-gas ratios as a function of stellar mass will only be amplified when accounting for the fact that gas fractions decrease with stellar mass at a given epoch (e.g. Narayanan et al 2015;Morokuma-Matsui & Baba 2015;Popping et al 2015;Scoville et al 2016;Saintonge et al 2011Saintonge et al , 2016Tacconi et al 2013Tacconi et al , 2017. Owing to the increased gas fraction of lower mass galaxies relative to more massive galaxies at a given redshift, the relation between dust mass to stellar mass will be shallower than that with dust-to-gas ratio.…”

Section: Metallicitymentioning

confidence: 99%

The Constant Average Relationship between Dust-obscured Star Formation and Stellar Mass from z = 0 to z = 2.5

Whitaker

Pope

Cybulski

et al. 2017

ApJ

183

194

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The total star formation budget of galaxies consists of the sum of the unobscured star formation, as observed in the rest-frame ultraviolet (UV), together with the obscured component that is absorbed and re-radiated by dust grains in the infrared. We explore how the fraction of obscured star formation depends on stellar mass for mass-complete samples of galaxies at 0 < z < 2.5. We combine GALEX and WISE photometry for SDSS-selected galaxies with the 3D-HST treasury program and Spitzer/MIPS 24µm photometry in the well-studied 5 extragalactic CANDELS fields. We find a strong dependence of the fraction of obscured star formation (f obscured =SFR IR /SFR UV+IR ) on stellar mass, with remarkably little evolution in this fraction with redshift out to z=2.5. 50% of star formation is obscured for galaxies with log(M/M ⊙ )=9.4; although unobscured star formation dominates the budget at lower masses, there exists a tail of low mass extremely obscured star-forming galaxies at z > 1. For log(M/M ⊙ )>10.5, >90% of star formation is obscured at all redshifts. We also show that at fixed total SFR, f obscured is lower at higher redshift. At fixed mass, high-redshift galaxies are observed to have more compact sizes and much higher star formation rates, gas fractions and hence surface densities (implying higher dust obscuration), yet we observe no redshift evolution in f obscured with stellar mass. This poses a challenge to theoretical models to reproduce, where the observed compact sizes at high redshift seem in tension with lower dust obscuration.

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“…Most surveys find that the mass in cold gas is highly dependent on the galaxies' stellar mass. For low-redshift galaxies (z < 0.5) the mass in HI (H2) ranges from 20 − 30% (8 − 10%) of the stellar mass for galaxies with M * = 10 10 M , dropping to 5 − 10% (4 − 5%) for galaxies with M * = 10 11 M (Saintonge et al 2011;Catinella et al 2013;Boselli et al 2014;Morokuma-Matsui & Baba 2015). Therefore, in order to estimate the mass of the cold gas component, we consider a cold gas fraction f cold which depends on the measured M * of our galaxies.…”

Section: Stars and Cold Gasmentioning

confidence: 99%

First test of Verlinde's theory of emergent gravity using weak gravitational lensing measurements

Brouwer

Visser

Dvornik

et al. 2016

Mon. Not. R. Astron. Soc.

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Verlinde (2016) proposed that the observed excess gravity in galaxies and clusters is the consequence of Emergent Gravity (EG). In this theory the standard gravitational laws are modified on galactic and larger scales due to the displacement of dark energy by baryonic matter. EG gives an estimate of the excess gravity (described as an apparent dark matter density) in terms of the baryonic mass distribution and the Hubble parameter. In this work we present the first test of EG using weak gravitational lensing, within the regime of validity of the current model. Although there is no direct description of lensing and cosmology in EG yet, we can make a reasonable estimate of the expected lensing signal of low redshift galaxies by assuming a background ΛCDM cosmology. We measure the (apparent) average surface mass density profiles of 33, 613 isolated central galaxies, and compare them to those predicted by EG based on the galaxies' baryonic masses. To this end we employ the ∼ 180 deg 2 overlap of the Kilo-Degree Survey (KiDS) with the spectroscopic Galaxy And Mass Assembly (GAMA) survey. We find that the prediction from EG, despite requiring no free parameters, is in good agreement with the observed galaxy-galaxy lensing profiles in four different stellar mass bins. Although this performance is remarkable, this study is only a first step. Further advancements on both the theoretical framework and observational tests of EG are needed before it can be considered a fully developed and solidly tested theory.

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Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

Cited by 21 publications

References 157 publications

Coevolution of metallicity and star formation in galaxies toz≃ 3.7 – II. A theoretical model

Coevolution of metallicity and star formation in galaxies toz≃ 3.7 – II. A theoretical model

The Constant Average Relationship between Dust-obscured Star Formation and Stellar Mass from z = 0 to z = 2.5

First test of Verlinde's theory of emergent gravity using weak gravitational lensing measurements

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