Exploring galaxy colour in different environments of the cosmic web with SDSS

Pandey, Biswajit; Sarkar, Suman

doi:10.1093/mnras/staa2772

Cited by 29 publications

(23 citation statements)

References 82 publications

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“…The dependence of galaxy properties with environment was firmly confirmed in the last decades due to the observations provided by wide galaxy surveys such as the Sloan Digital Sky Survey (York et al 2000, SDSS), Cosmic Evolution Survey (Scoville et al 2007, COSMOS) and the PRIsm MUlti-Object Survey (Coil et al 2011, PRIMUS). A bimodal distribution is found in galaxy color (Pandey & Sarkar 2020) and star formation rate (Wetzel et al 2012;Trussler et al 2020, SFR) as well.…”

Section: Introductionmentioning

confidence: 95%

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

Carvalho

Ferreras

Aragón-Salamanca

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a study of a sample of 254 clusters from the SDSS-DR7 Yang Catalog and an auxiliary sample of field galaxies to perform a detailed investigation on how galaxy quenching depends on both environment and galaxy stellar mass. Our samples are restricted to 0.03≤z≤0.1 and we only consider clusters with $\rm log(M_{halo}/M_{\odot }) \ge 14$. Comparing properties of field and cluster galaxies in the Blue Cloud, Green Valley and Red Sequence, we find evidence that field galaxies in the red sequence hosted star formation events $\rm 2.1 \pm 0.7$ Gyr ago, on average, more recently than galaxies in cluster environments. Dissecting the star formation rate vs stellar mass diagram we show how morphology rapidly changes after reaching the green valley region, while the star formation rate keeps decreasing. In addition, we use the relation between location in the projected phase space and infall time to explore the time delay between morphological and specific Star Formation Rate variations. We estimate that the transition from late to early-type morphology happens in $\rm \Delta t_{inf} \sim$1 Gyr, whereas the quenching of star formation takes ∼3 Gyr. The time-scale we estimate for morphological transitions is similar to the expected for the delayed-then-rapid quenching model. Therefore, we suggest that the delay phase is characterized mostly by morphological transition, which then contributes morphological quenching as an additional ingredient in galaxy evolution.

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Section: Introductionmentioning

confidence: 95%

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

Carvalho

Ferreras

Aragón-Salamanca

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Here, the local void [56], Virgo and Coma clusters act as major agents that shape the dynamics of nearby galaxies [57,58] and drive the buildup and assembly of the local galaxy population [59][60][61][62][63]. Such environmental effects are also seen in even larger volumes such as those of deep galaxy redshift surveys (e.g., [64][65][66]).…”

Section: Introductionmentioning

confidence: 99%

Caught in the cosmic web: Environmental effect on halo concentrations, shape, and spin

et al. 2021

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Using a set of high-resolution simulations we study the statistical correlation of dark matter halo properties with the large-scale environment. We consider halo populations split into four cosmic web (CW) elements: voids, walls, filaments, and nodes. For the first time we present a study of CW effects for halos covering six decades in mass: 10 8 -10 14 h −1 M ⊙ . We find that the fraction of halos living in various web components is a strong function of mass, with the majority of M > 10 12 h −1 M ⊙ halos living in filaments and nodes. Low mass halos are more equitably distributed in filaments, walls, and voids. For halo density profiles and formation times we find a universal mass threshold of M th ∼ 6 × 10 10 h −1 M ⊙ below which these properties vary with environment. Here, filament halos have the steepest concentrationmass relation, walls are close to the overall mean, and void halos have the flattest relation. This amounts to c 200 for filament and void halos that are, respectively, 14% higher and 7% lower than the mean at M ¼ 2 × 10 8 h −1 M ⊙ . We find double power-law fits that very well describe cðMÞ for the four environments in the whole probed mass range. A complementary picture is found for the average formation times, with the mass-formation time relations following trends shown for the concentrations: the nodes halos being the oldest and void halo the youngest. The CW environmental effect is much weaker when studying the halo spin and shapes. The trend with halo mass is reversed: the small halos with M < 10 10 h −1 M ⊙ seem to be unaffected by the CW environment. Some weak trends are visible for more massive void and wall halos, which, on average, are characterized by lower spin and higher triaxiality parameters.

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“…Several observational studies [72][73][74][75][76][77][78][79][80][81][82] show that the physical association between galaxy properties and environment extend much beyond the size of their host halo. In this work, we test if the colour of galaxies at fixed stellar mass and fixed morphology is sensitive to the large-scale environment.…”

Section: Discussionmentioning

confidence: 99%

“…The large-scale environmental dependence of galaxy properties may thus signal the existence of galaxy assembly bias. A large number of studies with different observational data sets indicate statistically significant correlations between the large-scale environment and different galaxy properties [72][73][74][75][76][77][78][79][80][81][82].…”

Section: Introductionmentioning

confidence: 99%

“…If the assembly history of spirals plays any role in determining their colour then the colour of these galaxies should depend on their large-scale environment at fixed mass and morphology. Recently, Pandey & Sarkar [80] analyze the SDSS data and find that the fraction of red and blue galaxies depend on their geometric environment at fixed density. The correlation between any galaxy property and the largescale environment can also be measured using the mutual information between them [79].…”

Section: Introductionmentioning

confidence: 99%

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On the origin of red spirals: Does assembly bias play a role?

Sarkar,

Pandey,

Das

2021

Preprint

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The formation of the red spirals is a puzzling issue in the standard picture of galaxy formation and evolution. Most studies attribute the colour of the red spirals to different environmental effects. We analyze a volume limited sample from the SDSS to study the roles of small-scale and large-scale environments on the colour of spiral galaxies. We compare the star formation rate, stellar age and stellar mass distributions of the red and blue spirals and find statistically significant differences between them at 99.9% confidence level. The red spirals inhabit significantly denser regions than the blue spirals, explaining some of the observed differences in their physical properties. However, the differences persist in all types of environments, indicating that the local density alone is not sufficient to explain the origin of the red spirals. Using an information theoretic framework, we find a small but non-zero mutual information between the colour of spiral galaxies and their large-scale environment that are statistically significant (99.9% confidence level) throughout the entire length scale probed. Such correlations between the colour and the large-scale environment of spiral galaxies may result from the assembly bias. Thus both the local environment and the assembly bias may play essential roles in forming the red spirals. The spiral galaxies may have different assembly histories across all types of environments. We propose a picture where the differences in the assembly histories may produce spiral galaxies with different cold gas content. Such a difference would make some spirals more susceptible to quenching. In all environments, the spirals with higher cold gas content could delay the quenching and maintain a bluer colour, whereas the spirals with lower cold gas fractions would be easily quenched and become red.

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Exploring galaxy colour in different environments of the cosmic web with SDSS

Cited by 29 publications

References 82 publications

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

Caught in the cosmic web: Environmental effect on halo concentrations, shape, and spin

On the origin of red spirals: Does assembly bias play a role?

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