Bulgeless galaxies in the COSMOS field: environment and star formation evolution at z &lt; 1

Grossi, M.; Fernandes, C. A. C.; Sobral, David; Afonso, J.; Telles, E.; Bizzocchi, L.; Paulino-Afonso, Ana; Matute, I.

doi:10.1093/mnras/stx3165

Cited by 13 publications

(17 citation statements)

References 118 publications

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“…Results tend to agree that higher density environments increase the fraction of quiescent (red) galaxies and we do see this in the COSMOS field (see top right panel of Figure 28; Peng et al 2010;McGee et al 2011;Scoville et al 2013;Darvish et al 2014Darvish et al , 2016. Whether or not the normalization of the MS (defined for starforming galaxies) depends on galaxy environment is still under debate, but many studies identify no variations of MS with environments such as clusters and voids, e.g., Tyler et al (2013), Koyama et al (2014), Ricciardelli et al (2014), Tyler et al (2014), Grossi et al (2018), Paulino-Afonso et al (2019), Pharo et al (2020 (although see Duivenvoorden et al 2016 who found a difference at 1.5 < z < 2 in COSMOS). However, at low redshift (z < 0.3), studies have reported a clear dependence of the MS on galaxy environment (e.g., von der Linden et al 2010, Haines et al 2013, Gu et al 2018, Paccagnella et al 2016).…”

Section: Environmental Trendssupporting

confidence: 73%

“…The fraction of star formation in irregular galaxies is roughly constant at around 20% in the three redshift bins shown but is slightly decreased in favor of galaxies classified as spheroidal for masses 10 11 M . Grossi et al (2018) found that, integrated over all luminosities, pure disk galaxies contribute significantly more to the cosmic SFRD at z < 1 and that the decline in sSFR with redshift is faster for bulge-dominated systems than for pure disks.…”

Section: Morphology Trendsmentioning

confidence: 95%

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The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Leslie

Schinnerer

Liu

et al. 2020

ApJ

111

143

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We provide a coherent, uniform measurement of the evolution of the logarithmic star formation rate (SFR) -stellar mass (M * ) relation, called the main sequence of star-forming galaxies (MS), for starforming and all galaxies out to z ∼ 5. We measure the MS using mean stacks of 3 GHz radio continuum images to derive average SFRs for ∼ 200,000 mass-selected galaxies at z > 0.3 in the COSMOS field. We describe the MS relation adopting a new model that incorporates a linear relation at low stellar mass (log(M * /M )<10) and a flattening at high stellar mass that becomes more prominent at low redshift (z < 1.5). We find that the SFR density peaks at 1.5 < z < 2 and at each epoch there is a characteristic stellar mass (M * = 1−4×10 10 M ) that contributes the most to the overall SFR density. This characteristic mass increases with redshift, at least to z ∼ 2.5. We find no significant evidence for variations in the MS relation for galaxies in different environments traced by the galaxy number density at 0.3 < z < 3, nor for galaxies in X-ray groups at z ∼ 0.75. We confirm that massive bulgedominated galaxies have lower SFRs than disk-dominated galaxies at a fixed stellar mass at z < 1.2. As a consequence, the increase in bulge-dominated galaxies in the local star-forming population leads to a flattening of the MS at high stellar masses. This indicates that "mass-quenching" is linked with changes in the morphological composition of galaxies at a fixed stellar mass.

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Section: Environmental Trendssupporting

confidence: 73%

Section: Morphology Trendsmentioning

confidence: 95%

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Leslie

Schinnerer

Liu

et al. 2020

ApJ

111

143

View full text Add to dashboard Cite

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“…Lackner & Gunn 2013). At intermediate redshifts (z ∼ 0.4−0.8), Grossi et al (2018) find that a sample of Hα-selected galaxies tend to have more prominent bulges in higher-density environments. However, we lack observations of the environmental dependence of the bulge prevalence at these redshifts for a continuum-selected sample.…”

Section: Introductionmentioning

confidence: 76%

VIS³COS

Paulino-Afonso

Sobral

Darvish

et al. 2019

A&A

Self Cite

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We study the impact of local density and stellar mass on the structure and morphology of approximately 500 quiescent and star-forming galaxies from the VIMOS Spectroscopic Survey of a Superstructure in COSMOS (VIS3COS). We perform bulge-to-disc decomposition of the surface brightness profiles and find ∼41 ± 3% of > 1010 M⊙ galaxies to be best fitted with two components. We complement our analysis with non-parametric morphological measurements and qualitative visual classifications. We find that both galaxy structure and morphology depend on stellar mass and environment for our sample as a whole. We only find an impact of the environment on galaxy size for galaxies more massive than 1011 M⊙. We find higher Sérsic indices (n) and bulge-to-total ratios (B/T) in high-density regions when compared to low-density counterparts at similar stellar masses. We also find that galaxies with higher stellar mass have steeper light profiles (high n, B/T) compared to galaxies with lower stellar mass. Using visual classifications, we find a morphology–density relation at z ∼ 0.84 for galaxies more massive than 1010 M⊙, with elliptical galaxies being dominant at high-density regions and disc galaxies more common in low-density regions. However, when splitting the sample into colour–colour-selected star-forming and quiescent sub-populations, there are no statistically significant differences between low- and high-density regions. We find that quiescent galaxies are smaller, have higher Sérsic indices (for single profiles, around n ∼ 4), and higher bulge-to-total light ratios (for decomposed profiles, around B/T ∼ 0.5) when compared to star-forming counterparts (n ∼ 1 and B/T ∼ 0.3, for single and double profiles, respectively). We confirm these trends with non-parametric quantities, finding quiescent galaxies to be smoother (lower asymmetry, lower M20) and to have most of their light over smaller areas (higher concentration and Gini coefficient) than star-forming galaxies. Overall, we find a stronger dependence of structure and morphology on stellar mass than on local density and these relations are strongly correlated with the quenching fraction. The change in average structure or morphology corresponds to a change in the relative fractions of blue disc-like galaxies and red elliptical galaxies with stellar mass and environment. We hypothesise that the processes responsible for the quenching of star formation must also affect the galaxy morphology on similar timescales.

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“…These relations have been extensively studied in the local universe (Blanton & Moustakas 2009), and have been explored at high redshifts using several deep field survey data ⋆ E-mail: hhwang@kasi.re.kr † E-mail: jhshin@kasi.re.kr ‡ E-mail: hmsong@kasi.re.kr (e.g. Cucciati et al 2006;Cooper et al 2007;Grossi et al 2018;Pelliccia et al 2019). Understanding this environmental dependence of galaxy properties and its evolution with redshift is very important in modern astrophysics because it provides strong constraints on the model of galaxy formation and evolution (Peng et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Evolution of star formation rate–density relation over cosmic time in a simulated universe: the observed reversal reproduced

Hwang

Shin

Song

2019

Monthly Notices of the Royal Astronomical Society

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We use the IllustrisTNG cosmological hydrodynamical simulation to study the evolution of star formation rate (SFR)-density relation over cosmic time. We construct several samples of galaxies at different redshifts from z = 2.0 to z = 0.0, which have the same comoving number density. The SFR of galaxies decreases with local density at z = 0.0, but its dependence on local density becomes weaker with redshift. At z 1.0, the SFR of galaxies increases with local density (reversal of the SFRdensity relation), and its dependence becomes stronger with redshift. This change of SFR-density relation with redshift still remains even when fixing the stellar masses of galaxies. The dependence of SFR on the distance to a galaxy cluster also shows a change with redshift in a way similar to the case based on local density, but the reversal happens at a higher redshift, z ∼ 1.5, in clusters. On the other hand, the molecular gas fraction always decreases with local density regardless of redshift at z = 0.0 − 2.0 even though the dependence becomes weaker when we fix the stellar mass. Our study demonstrates that the observed reversal of the SFR-density relation at z 1.0 can be successfully reproduced in cosmological simulations. Our results are consistent with the idea that massive, star-forming galaxies are strongly clustered at high redshifts, forming larger structures. These galaxies then consume their gas faster than those in low-density regions through frequent interactions with other galaxies, ending up being quiescent in the local universe.

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Bulgeless galaxies in the COSMOS field: environment and star formation evolution at z < 1

Cited by 13 publications

References 118 publications

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

VIS³COS

Evolution of star formation rate–density relation over cosmic time in a simulated universe: the observed reversal reproduced

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