scholarly journals Evolution of the distribution of stellar mass and light since redshift of unity

2012 ◽  
Vol 8 (S295) ◽  
pp. 121-124
Author(s):  
Cheng Li
Keyword(s):  
Dark Matter ◽  
Spatial Scale ◽  
Galaxy Formation ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Local Universe ◽  
Sky Survey ◽  
Fluctuation Amplitude ◽  
Better Than ◽  
Environmental Dependence

AbstractWe use data from the Sloan Digital Sky Survey (SDSS) and the DEEP2 survey to characterize the distribution of stellar mass and light of galaxies in the low-redshift and z = 1 Universe. We investigate the clustering bias of stellar mass and light by comparing these to projected autocorrelations of dark matter estimated from the Millennium Simulations (MS). All of the autocorrelation and bias functions show systematic trends with spatial scale and waveband, which are impressively similar at the two redshifts. This shows that the well-established environmental dependence of stellar populations in the local Universe is already in place at z = 1. The recent MS-based galaxy formation simulation of Guo et al. (2011) reproduces the scale-dependent clustering of luminosity to an accuracy better than 30% in all bands and at both redshifts, but substantially overpredicts mass autocorrelations at separations below ~ 2 Mpc. Further comparison of the shapes of our stellar mass bias functions with those predicted by the model suggests that both the SDSS and DEEP2 data prefer a fluctuation amplitude of σ8 ~ 0.8 rather than the σ8 = 0.9 assumed by the MS.

scholarly journals How dark are filaments in the cosmic web?

2020 ◽  
Vol 498 (3) ◽  
pp. 3158-3170
Author(s):  
Tianyi Yang ◽  
Michael J Hudson ◽  
Niayesh Afshordi
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Cold Dark Matter ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Weak Lensing ◽  
Sky Survey ◽  
Mass Fractions ◽  
The Masses ◽  
Red Galaxies

ABSTRACT The cold dark matter model predicts that dark matter haloes are connected by filaments. Direct measurements of the masses and structure of these filaments are difficult, but recently several studies have detected these dark-matter-dominated filaments using weak lensing. Here we study the efficiency of galaxy formation within the filaments by measuring their total mass-to-light ratios and stellar mass fractions. Specifically, we stack pairs of luminous red galaxies (LRGs) with a typical separation on the sky of 8 h−1 Mpc. We stack background galaxy shapes around pairs to obtain mass maps through weak lensing, and we stack galaxies from the Sloan Digital Sky Survey to obtain maps of light and stellar mass. To isolate the signal from the filament, we construct two matched catalogues of physical and non-physical (projected) LRG pairs, with the same distributions of redshift and separation. We then subtract the two stacked maps. Using LRG pair samples from the Baryon Oscillation Spectroscopic Survey at two different redshifts, we find that the evolution of the mass in filament is consistent with the predictions from perturbation theory. The filaments are not entirely dark: Their mass-to-light ratios (M/L = 351 ± 137 in solar units in the rband) and stellar mass fractions (Mstellar/M = 0.0073 ± 0.0030) are consistent with the cosmic values (and with their redshift evolutions).

scholarly journals Modelling the tightest relation between galaxy properties and dark matter halo properties from hydrodynamical simulations of galaxy formation

2020 ◽  
Vol 493 (3) ◽  
pp. 4453-4462
Author(s):  
Jian-hua He
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Dark Matter Halo ◽  
Strong Interactions ◽  
Circular Velocity ◽  
Sky Survey ◽  
Hydrodynamical Simulations ◽  
Robust Prediction

ABSTRACT We investigate how a property of a galaxy correlates most tightly with a property of its host dark matter halo, using state-of-the-art hydrodynamical simulations of galaxy formation: EAGLE, Illustris, and IllustrisTNG. Unlike most of the previous work, our analyses focus on all types of galaxies, including both central and satellite galaxies. We find that the stellar mass of a galaxy at the epoch of the peak circular velocity with an evolution correction gives the tightest such correlation to the peak circular velocity Vpeak of the galaxy’s underling dark matter halo. The evolution of galaxy stellar mass reduces rather than increases scatter in such a relation. We also find that one major source of scatter comes from star stripping due to the strong interactions between galaxies. Even though, we show that the size of scatter predicted by hydrodynamical simulations has a negligible impact on the clustering of dense Vpeak-selected subhalo from simulations, which suggests that even the simplest subhalo abundance matching (SHAM), without scatter and any additional free parameter, can provide a robust prediction of galaxy clustering that can agree impressively well with the observations from the Sloan Digital Sky Survey (SDSS) main galaxy survey.

scholarly journals The weak imprint of environment on the stellar populations of galaxies

2020 ◽  
Vol 500 (4) ◽  
pp. 4469-4490 ◽  
Author(s):  
James Trussler ◽  
Roberto Maiolino ◽  
Claudia Maraston ◽  
Yingjie Peng ◽  
Daniel Thomas ◽  
...  
Keyword(s):  
Environmental Effects ◽  
Unique Feature ◽  
Stellar Populations ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Star Forming ◽  
Sky Survey ◽  
Satellite Galaxies ◽  
Projected Distance ◽  
Environmental Dependence

ABSTRACT We investigate the environmental dependence of the stellar populations of galaxies in Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Echoing earlier works, we find that satellites are both more metal-rich (<0.1 dex) and older (<2 Gyr) than centrals of the same stellar mass. However, after separating star-forming, green valley, and passive galaxies, we find that the true environmental dependence of both stellar metallicity (<0.03 dex) and age (<0.5 Gyr) is in fact much weaker. We show that the strong environmental effects found when galaxies are not differentiated result from a combination of selection effects brought about by the environmental dependence of the quenched fraction of galaxies, and thus we strongly advocate for the separation of star-forming, green valley, and passive galaxies when the environmental dependence of galaxy properties are investigated. We also study further environmental trends separately for both central and satellite galaxies. We find that star-forming galaxies show no environmental effects, neither for centrals nor for satellites. In contrast, the stellar metallicities of passive and green valley satellites increase weakly (<0.05 and <0.08 dex, respectively) with increasing halo mass, increasing local overdensity and decreasing projected distance from their central; this effect is interpreted in terms of moderate environmental starvation (‘strangulation’) contributing to the quenching of satellite galaxies. Finally, we find a unique feature in the stellar mass–stellar metallicity relation for passive centrals, where galaxies in more massive haloes have larger stellar mass (∼0.1 dex) at constant stellar metallicity; this effect is interpreted in terms of dry merging of passive central galaxies and/or progenitor bias.

scholarly journals Revealing galactic scale bars with the help of Galaxy Zoo

2012 ◽  
Vol 10 (H16) ◽  
pp. 324-324
Author(s):  
Karen L. Masters ◽  
Keyword(s):  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Gas Content ◽  
Barred Galaxies ◽  
Sky Survey ◽  
The Galaxy ◽  
Galaxy Sample ◽  
External Sources ◽  
Disc Galaxies ◽  
Environmental Dependence

AbstractWe use visual classifications of the brightest 250,000 galaxies in the Sloan Digital Sky Survey Main Galaxy Sample provided by citizen scientists via the Galaxy Zoo project (www.galaxyzoo.org, Lintott et al. 2008) to identify a sample of local disc galaxies with reliable bar identifications.These data, combined with information on the atomic gas content from the ALFALFA survey (Haynes et al. 2011) show that disc galaxies with higher gas content have lower bar fractions.We use a gas deficiency parameter to show that disc galaxies with more/less gas than expected for their stellar mass are less/more likely to host bars. Furthermore, we see that at a fixed gas content there is no residual correlation between bar fraction and stellar mass. We argue that this suggests previously observed correlations between galaxy colour/stellar mass and (strong) bar fraction (e.g. from the sample in Masters et al. 2011, and also see Nair & Abraham 2010) could be driven by the interaction between bars and the gas content of the disc, since more massive, optically redder disc galaxies are observed to have lower gas contents.Furthermore we see evidence that at a fixed gas content the global colours of barred galaxies are redder than those of unbarred galaxies. We suggest that this could be due to the exchange of angular momentum beyond co-rotation which might stop a replenishment of gas from external sources, and act as a source of feedback to temporarily halt or reduce the star formation in the outer parts of barred discs.These results (published as Masters et al. 2012) combined with those of Skibba et al. (2012), who use the same sample to show a clear (but subtle and complicated) environmental dependence of the bar fraction in disc galaxies, suggest that bars are intimately linked to the evolution of disc galaxies.

scholarly journals Constraining scatter in the stellar mass–halo mass relation for haloes less massive than the Milky Way

2019 ◽  
Vol 488 (4) ◽  
pp. 4916-4925 ◽  
Author(s):  
Magdelena Allen ◽  
Peter Behroozi ◽  
Chung-Pei Ma
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Stellar Mass ◽  
Distribution Functions ◽  
Sloan Digital Sky Survey ◽  
Data Sets ◽  
Mass Relation ◽  
Velocity Distribution Functions ◽  
Halo Masses ◽  
Stellar Masses

ABSTRACT Most galaxies are hosted by massive, invisible dark matter haloes, yet little is known about the scatter in the stellar mass–halo mass relation for galaxies with host halo masses Mh ≤ 1011M⊙. Using mock catalogues based on dark matter simulations, we find that two observable signatures are sensitive to scatter in the stellar mass–halo mass relation even at these mass scales; i.e. conditional stellar mass functions and velocity distribution functions for neighbouring galaxies. We compute these observables for  179,373 galaxies in the Sloan Digital Sky Survey (SDSS) with stellar masses M* > 109 M⊙ and redshifts 0.01 < z < 0.307. We then compare to mock observations generated from the Bolshoi-Planck dark matter simulation for stellar mass–halo mass scatters ranging from 0 to 0.6 dex. The observed results are consistent with simulated results for most values of scatter (<0.6 dex), and SDSS statistics are insufficient to provide firm constraints. However, this method could provide much tighter constraints on stellar mass–halo mass scatter in the future if applied to larger data sets, especially the anticipated Dark Energy Spectroscopic Instrument Bright Galaxy Survey. Constraining the value of scatter could have important implications for galaxy formation and evolution.

THE DISTRIBUTION OF STELLAR MASS-TO-LIGHT RATIO IN THE LOCAL UNIVERSE

2011 ◽  
Vol 20 (10) ◽  
pp. 2105-2108
Author(s):  
CHENG LI
Keyword(s):  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Distribution Models ◽  
Quantitative Characterization ◽  
Local Universe ◽  
Sky Survey ◽  
The Mean ◽  
Halo Occupation Distribution ◽  
Mass Functions

We have used the final data release of the Sloan Digital Sky Survey (SDSS) to estimate the projected autocorrelation function, wp(rp), for the stellar mass of galaxies, as well as their stellar light in the SDSS five photometric bands. All these quantities are robustly and precisely determined over scales 10h-1 kpc < rp < 30h-1 Mpc . Ratios of wp(rp) between two given wavebands are proportional to the mean color of correlated stars at rp from a randomly chosen star, while the ratio of stellar mass to luminosity autocorrelations measures an analogous mean stellar mass-to-light ratio (M*/L). These measurements provide a precise quantitative characterization of the well-known dependence of stellar populations on environment, which, when combined with accurate luminosity and stellar mass functions, is expected to provide a compact way to constrain Halo Occupation Distribution models that try to represent all the correlations in detail.

scholarly journals The quantity of dark matter in early-type galaxies and its relation to the environment

2019 ◽  
Vol 488 (1) ◽  
pp. 1320-1331 ◽  
Author(s):  
A Nigoche-Netro ◽  
G Ramos-Larios ◽  
P Lagos ◽  
E de la Fuente ◽  
A Ruelas-Mayorga ◽  
...  
Keyword(s):  
Dark Matter ◽  
Surface Brightness ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Early Type ◽  
Dynamical Mass ◽  
Redshift Range ◽  
Sky Survey ◽  
The Impact ◽  
Mass Functions

ABSTRACT We study the behaviour of the dynamical and stellar mass inside the effective radius of early-type galaxies (ETGs) as a function of environment considering Newtonian dynamics, different surface-brightness profiles, different initial mass functions (IMF), and different redshift ranges. We use several samples of ETGs – ranging from 19 000 to 98 000 objects – from the ninth data release of the Sloan Digital Sky Survey. We assume that any difference between the dynamical and stellar mass is due to dark matter and/or a non-universal IMF. The main results, considering samples in the redshift range 0.0024 ≤ z ≤ 0.35, are as follows: (i) the amount of dark matter inside ETGs depends on the environment; (ii) ETGs in low-density environments span a wider dark matter range than ETGs in dense environments; (iii) the amount of dark matter inside ETGs in the most dense environments will be less than approximately 55–75 per cent of the dynamical mass; (iv) the accurate value of this upper limit depends on the impact of the IMF on the stellar mass estimation; (v) in the case of an ETG sample which is approximately complete for log(MVirial/MSun) > 10.5 and in the redshift range 0.04 ≤ z ≤ 0.08, we find that the amount of dark matter in the most dense environments will be less than approximately 60–65 per cent of the dynamical mass.

scholarly journals Age-density relation of Main galaxies at fixed parameters or for different galaxy families

Open Physics ◽  
2015 ◽  
Vol 13 (1) ◽  
Author(s):  
Xin-Fa Deng ◽  
Jun Song ◽  
Yi-Qing Chen ◽  
Peng Jiang ◽  
Ying-Ping Ding
Keyword(s):  
Morphological Type ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
Density Relation ◽  
Blue Galaxies ◽  
The One ◽  
Red Galaxies ◽  
Density Regime ◽  
Environmental Dependence

AbstractUsing two volume-limited Main galaxy samples of the Sloan Digital Sky Survey Data Release 10 (SDSS DR10), we examine the environmental dependence of galaxy age at fixed parameters or for different galaxy families. Statistical results show that the environmental dependence of galaxy age is stronger for late type galaxies, but can be still observed for the early types: the age of galaxies in the densest regime is preferentially older than that in the lowest density regime with the same morphological type. We also find that the environmental dependence of galaxy age for red galaxies and Low Stellar Mass (LSM) galaxies is stronger, while the one for blue galaxies and High Stellar Mass ( HSM ) galaxies is very weak.

scholarly journals THE ENVIRONMENTAL DEPENDENCE OF GALAXY AGE AND STELLAR MASS IN THE REDSHIFT REGION 0.6 ≤ z ≤ 0.75

2019 ◽  
Vol 55 (2) ◽  
pp. 185-191
Author(s):  
Xin-Fa Deng
Keyword(s):  
Survey Data ◽  
Local Environment ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
Data Release ◽  
Galaxy Sample ◽  
Environmental Dependence

In this work, I construct a LRG (Luminous Red Galaxy) sample with redshifts 0.6 ≤ z ≤ 0.75 from the Sloan Digital Sky Survey Data Release 15 (SDSS DR15), which contains 184172 CMASS LRGs and 27158 eBOSS LRGs, and examine the environmental dependence of galaxy age and stellar mass in this galaxy sample. I divide this LRG sample into subsamples with a redshift binning size of ∆z = 0.01, and analyze the environmental dependence of galaxy age and stellar mass for these subsamples in each redshift bin. Overall, galaxy age and stellar mass in the LRG sample with redshift 0.6 ≤ z ≤ 0.75 are very weakly correlated with the local environment, which shows that minimal environmental dependence of galaxy parameters can continue to larger redshifts.

Environmental dependence of stellar mass for SDSS-III/BOSS galaxies

2014 ◽  
Vol 92 (1) ◽  
pp. 36-40 ◽  
Author(s):  
Xin-Fa Deng ◽  
Si-Yu Zou
Keyword(s):  
Selection Effect ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
Data Release ◽  
Galaxy Sample ◽  
Environmental Dependence

Using the LOWZ (0.15 ≤ z ≤ 0.43) and CMASS (0.43 ≤ z ≤ 0.7) galaxy samples of the ninth data release from the Sloan Digital Sky Survey (SDSS) III Baryon Oscillation Spectroscopic Survey (BOSS), we investigate the environmental dependence of stellar mass of BOSS galaxies, and conclude that like the luminous red galaxy sample of the SDSS, the environmental dependence of stellar mass of BOSS galaxies is fairly weak. Results of this work also show that the CMASS sample with the redshift 0.43 ≤ z ≤ 0.7 used by many authors seriously suffers from the radial selection effect.

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