scholarly journals Virial Halo Mass Function in the Planck Cosmology

2021 ◽  
Vol 922 (1) ◽  
pp. 89
Author(s):  
Masato Shirasaki ◽  
Tomoaki Ishiyama ◽  
Shin’ichiro Ando
Keyword(s):  
Luminosity Function ◽  
Mass Function ◽  
Number Density ◽  
Baseline Model ◽  
Wide Range ◽  
Halo Masses ◽  
Number Counts ◽  
Mass Functions ◽  
Analytic Prediction ◽  
Fitting Parameters

Abstract We study halo mass functions with high-resolution N-body simulations under a ΛCDM cosmology. Our simulations adopt the cosmological model that is consistent with recent measurements of the cosmic microwave backgrounds with the Planck satellite. We calibrate the halo mass functions for 108.5 ≲ M vir/(h −1 M ⊙) ≲ 1015.0–0.45 z , where M vir is the virial spherical-overdensity mass and redshift z ranges from 0 to 7. The halo mass function in our simulations can be fitted by a four-parameter model over a wide range of halo masses and redshifts, while we require some redshift evolution of the fitting parameters. Our new fitting formula of the mass function has a 5%-level precision, except for the highest masses at z ≤ 7. Our model predicts that the analytic prediction in Sheth & Tormen would overestimate the halo abundance at z = 6 with M vir = 108.5–10 h −1 M ⊙ by 20%–30%. Our calibrated halo mass function provides a baseline model to constrain warm dark matter (WDM) by high-z galaxy number counts. We compare a cumulative luminosity function of galaxies at z = 6 with the total halo abundance based on our model and a recently proposed WDM correction. We find that WDM with its mass lighter than 2.71 keV is incompatible with the observed galaxy number density at a 2σ confidence level.

The K-Band Luminosity Function of Galaxies

1998 ◽  
Vol 179 ◽  
pp. 278-280
Author(s):  
J. P. Gardner ◽  
R. M. Sharples ◽  
C. S. Frenk ◽  
B. E. Carrasco
Keyword(s):  
Luminosity Function ◽  
Near Infrared ◽  
Mass Function ◽  
Solar Mass ◽  
The Galaxy ◽  
Statistical Studies ◽  
The Absolute ◽  
Number Counts ◽  
Luminosity Evolution ◽  
K Band

The luminosity function of galaxies is central to many problems in cosmology, including the interpretation of faint number counts. The near-infrared provides several advantages over the optical for statistical studies of galaxies, including smooth and well-understood K-corrections and expected luminosity evolution. The K–band is dominated by near-solar mass stars which make up the bulk of the galaxy. The absolute K magnitude is a measure of the visible mass in a galaxy, and thus the K–band luminosity function is an observational counterpart of the mass function of galaxies.

scholarly journals The XXL Survey

2018 ◽  
Vol 620 ◽  
pp. A7 ◽  
Author(s):  
V. Guglielmo ◽  
B. M. Poggianti ◽  
B. Vulcani ◽  
C. Adami ◽  
F. Gastaldello ◽  
...  
Keyword(s):  
Mass Function ◽  
Stellar Mass ◽  
X Ray ◽  
Field Versus ◽  
Final Sample ◽  
Wide Range ◽  
The Galaxy ◽  
Halo Masses ◽  
Stellar Masses ◽  
Physical Phenomena

Context. The fraction of galaxies bound in groups in the nearby Universe is high (50% at z ~ 0). Systematic studies of galaxy properties in groups are important in order to improve our understanding of the evolution of galaxies and of the physical phenomena occurring within this environment. Aims. We have built a complete spectrophotometric sample of galaxies within X-ray detected, optically spectroscopically confirmed groups and clusters (G&C), covering a wide range of halo masses at z ≤ 0.6. Methods. In the context of the XXL survey, we analyse a sample of 164 G&C in the XXL-North region (XXL-N), at z ≤ 0.6, with a wide range of virial masses (1.24 × 1013 ≤ M500,scal(M⊙) ≤ 6.63 × 1014) and X-ray luminosities ((2.27 × 1041 ≤ L500,scalXXL(erg s−1) ≤ 2.15 × 1044)). The G&C are X-ray selected and spectroscopically confirmed. We describe the membership assignment and the spectroscopic completeness analysis, and compute stellar masses. As a first scientific exploitation of the sample, we study the dependence of the galaxy stellar mass function (GSMF) on global environment. Results. We present a spectrophotometric characterisation of the G&C and their galaxies. The final sample contains 132 G&C, 22 111 field galaxies and 2225 G&C galaxies with r-band magnitude <20. Of the G&C, 95% have at least three spectroscopic members, and 70% at least ten. The shape of the GSMF seems not to depend on environment (field versus G&C) or X-ray luminosity (used as a proxy for the virial mass of the system). These results are confirmed by the study of the correlation between mean stellar mass of G&C members and L500,scalXXL. We release the spectrophotometric catalogue of galaxies with all the quantities computed in this work. Conclusions. As a first homogeneous census of galaxies within X-ray spectroscopically confirmed G&C at these redshifts, this sample will allow environmental studies of the evolution of galaxy properties.

scholarly journals The COSMOS-UltraVISTA stellar-to-halo mass relationship: new insights on galaxy formation efficiency out to z ∼ 5

2019 ◽  
Vol 486 (4) ◽  
pp. 5468-5481 ◽  
Author(s):  
L Legrand ◽  
H J McCracken ◽  
I Davidzon ◽  
O Ilbert ◽  
J Coupon ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Mass Function ◽  
Stellar Mass ◽  
Steady Increase ◽  
Mass Measurements ◽  
Massive Galaxies ◽  
Sources Of Uncertainty ◽  
Wide Range ◽  
Halo Masses ◽  
Formation Efficiency

Abstract Using precise galaxy stellar mass function measurements in the COSMOS field we determine the stellar-to-halo mass relationship (SHMR) using a parametric abundance matching technique. The unique combination of size and highly complete stellar mass estimates in COSMOS allows us to determine the SHMR over a wide range of halo masses from z ∼ 0.2 to 5. At z ∼ 0.2, the ratio of stellar-to-halo mass content peaks at a characteristic halo mass Mh = 1012M⊙ and declines at higher and lower halo masses. This characteristic halo mass increases with redshift reaching Mh = 1012.5M⊙ at z ∼ 2.3 and remaining flat up to z = 4. We considered the principal sources of uncertainty in our stellar mass measurements and also the variation in halo mass estimates in the literature. We show that our results are robust to these sources of uncertainty and explore likely explanation for differences between our results and those published in the literature. The steady increase in characteristic halo mass with redshift points to a scenario where cold gas inflows become progressively more important in driving star formation at high redshifts, but larger samples of massive galaxies are needed to rigorously test this hypothesis.

scholarly journals The Substellar Luminosity and Mass Functions of the Trapezium Cluster Down to the Deuterium Burning Limit

2003 ◽  
Vol 211 ◽  
pp. 67-68
Author(s):  
August A. Muench ◽  
Elizabeth A. Lada ◽  
Charles J. Lada ◽  
João F. Alves
Keyword(s):  
Monte Carlo ◽  
Luminosity Function ◽  
Mass Function ◽  
Initial Mass Function ◽  
Secondary Peak ◽  
Brown Dwarf ◽  
Stellar Objects ◽  
Monte Carlo Calculations ◽  
Stellar Initial Mass Function ◽  
Mass Functions

We have employed an advanced suite of Monte Carlo calculations to model the infrared luminosity function (KLF) of the Trapezium cluster and to derive its Sub-stellar Initial Mass Function down to the deuterium burning limit. Independent of the details, we find that sub-stellar objects can account for no more than ~ 22% of the total number of likely cluster members. This cluster's substellar IMF steadily declines in a power-law fashion over most of the brown dwarf regime, however the formation of a secondary peak in the cluster's substellar KLF suggests the existence of a corresponding secondary peak in the substellar IMF between 10 and 30 times the mass of Jupiter based upon the seemingly degenerate behavior of the theoretical substellar mass-luminosity relation.

scholarly journals Mass and Spatial Distributions of Subhaloes in ΛCDM Cosmological Simulations

2006 ◽  
Vol 2 (S235) ◽  
pp. 127-127
Author(s):  
P. Nurmi ◽  
P. Heinämäki ◽  
J. Holopainen ◽  
P. Pihajoki ◽  
E. Saar ◽  
...  
Keyword(s):  
Spatial Distribution ◽  
Mass Fraction ◽  
Mass Function ◽  
Spatial Distributions ◽  
A Value ◽  
Lower Amplitude ◽  
Mass Fractions ◽  
Average Distribution ◽  
Halo Masses ◽  
Mass Functions

AbstractWe study subhalo populations surrounding massive dark matter haloes by using three AMIGA simulations each having different mass and spatial resolutions. Our analysis shows that the slope of the subhalo mass function has a value 0.9, which agrees with previous studies. The dependence of mass functions on redshift is the same for subhaloes and main haloes. In all simulations, combined subhalo masses are about 0.1-0.2 of main halo masses and this mass fraction increases slightly with redshift and the mass of the main halo. The distribution of mass fractions for subhaloes is close to Gaussian at z = 0 and differs slightly at earlier epochs. Spatial distribution of subhaloes as measured in units of virial radius Rvir of the main halo does not depend on redshift and follows r1/3 rule. Spatial distribution of all haloes surrounding main haloes continues up to 3 times Rvir with equal slope but lower amplitude. Beyond 16 times Rvir, the average distribution of haloes becomes uniform.

scholarly journals A lack of evolution in the very bright end of the galaxy luminosity function from z ≃ 8 to 10

2020 ◽  
Vol 493 (2) ◽  
pp. 2059-2084 ◽  
Author(s):  
R A A Bowler ◽  
M J Jarvis ◽  
J S Dunlop ◽  
R J McLure ◽  
D J McLeod ◽  
...  
Keyword(s):  
Galaxy Evolution ◽  
Luminosity Function ◽  
Near Infrared ◽  
Good Description ◽  
Number Density ◽  
Photometric Redshifts ◽  
Star Forming ◽  
Photometric Redshift ◽  
Wide Range ◽  
Best Fitting

ABSTRACT We utilize deep near-infrared survey data from the UltraVISTA fourth data release (DR4) and the VIDEO survey, in combination with overlapping optical and Spitzer data, to search for bright star-forming galaxies at z ≳ 7.5. Using a full photometric redshift fitting analysis applied to the ∼6 $\, {\rm deg}^2$ of imaging searched, we find 27 Lyman break galaxies (LBGs), including 20 new sources, with best-fitting photometric redshifts in the range 7.4 &lt; z &lt; 9.1. From this sample, we derive the rest-frame UV luminosity function at z = 8 and z = 9 out to extremely bright UV magnitudes (MUV ≃ −23) for the first time. We find an excess in the number density of bright galaxies in comparison to the typically assumed Schechter functional form derived from fainter samples. Combined with previous studies at lower redshift, our results show that there is little evolution in the number density of very bright (MUV ∼ −23) LBGs between z ≃ 5 and z ≃ 9. The tentative detection of an LBG with best-fitting photometric redshift of z = 10.9 ± 1.0 in our data is consistent with the derived evolution. We show that a double power-law fit with a brightening characteristic magnitude (ΔM*/Δz ≃ −0.5) and a steadily steepening bright-end slope (Δβ/Δz ≃ −0.5) provides a good description of the z &gt; 5 data over a wide range in absolute UV magnitude (−23 &lt; MUV &lt; −17). We postulate that the observed evolution can be explained by a lack of mass quenching at very high redshifts in combination with increasing dust obscuration within the first ${\sim}1 \, {\rm Gyr}$ of galaxy evolution.

scholarly journals The bolometric quasar luminosity function at z = 0–7

2020 ◽  
Vol 495 (3) ◽  
pp. 3252-3275 ◽  
Author(s):  
Xuejian Shen ◽  
Philip F Hopkins ◽  
Claude-André Faucher-Giguère ◽  
D M Alexander ◽  
Gordon T Richards ◽  
...  
Keyword(s):  
Luminosity Function ◽  
Mass Density ◽  
High Redshift ◽  
Late Phase ◽  
Mass Function ◽  
Evolutionary Pattern ◽  
Hierarchical Assembly ◽  
Best Fitting ◽  
Mass Functions ◽  
Photoionization Rate

ABSTRACT In this paper, we provide updated constraints on the bolometric quasar luminosity function (QLF) from z = 0 to z = 7. The constraints are based on an observational compilation that includes observations in the rest-frame IR, B band, UV, soft, and hard X-ray in past decades. Our method follows Hopkins et al. with an updated quasar SED model and bolometric and extinction corrections. The new best-fitting bolometric quasar luminosity function behaves qualitatively different from the old Hopkins model at high redshift. Compared with the old model, the number density normalization decreases towards higher redshift and the bright-end slope is steeper at z ≳ 2. Due to the paucity of measurements at the faint end, the faint end slope at z ≳ 5 is quite uncertain. We present two models, one featuring a progressively steeper faint-end slope at higher redshift and the other featuring a shallow faint-end slope at z ≳ 5. Further multiband observations of the faint-end QLF are needed to distinguish between these models. The evolutionary pattern of the bolometric QLF can be interpreted as an early phase likely dominated by the hierarchical assembly of structures and a late phase likely dominated by the quenching of galaxies. We explore the implications of this model on the ionizing photon production by quasars, the CXB spectrum, the SMBH mass density, and mass functions. The predicted hydrogen photoionization rate contributed by quasars is subdominant during the epoch of reionization and only becomes important at z ≲ 3. The predicted CXB spectrum, cosmic SMBH mass density, and SMBH mass function are generally consistent with existing observations.

scholarly journals The normalization and slope of the dark matter (sub-)halo mass function on sub-galactic scales

2020 ◽  
Vol 493 (1) ◽  
pp. 1268-1276
Author(s):  
Andrew J Benson
Keyword(s):  
Dark Matter ◽  
Gravitational Lensing ◽  
Cold Dark Matter ◽  
Mass Range ◽  
Mass Function ◽  
Matter Content ◽  
Dark Matter Halo ◽  
Halo Masses ◽  
Near Future ◽  
Mass Functions

ABSTRACT Simulations of cold dark matter make robust predictions about the slope and normalization of the dark matter halo and subhalo mass functions on small scales. Recent observational advances utilizing strong gravitational lensing have demonstrated the ability of this technique to place constraints on these quantities on subgalactic scales corresponding to dark matter halo masses of 106–$10^9\, \mathrm{M}_\odot$. On these scales the physics of baryons, which make up around 17 per cent of the matter content of the Universe but which are not included in pure dark matter N-body simulations, are expected to affect the growth of structure and the collapse of dark matter haloes. In this work, we develop a semi-analytic model to predict the amplitude and slope of the dark matter halo and subhalo mass functions on subgalactic scales in the presence of baryons. We find that the halo mass function is suppressed by up to 25 per cent, and the slope is modified, ranging from −1.916 to −1.868 in this mass range. These results are consistent with current measurements, but differ sufficiently from the expectations for a dark matter only universe that it may be testable in the near future.

scholarly journals New constraints on reionization from a redshift-independent efficiency model

2019 ◽  
Vol 15 (S352) ◽  
pp. 70-70
Author(s):  
Rohan Potham Naidu
Keyword(s):  
Star Formation ◽  
Luminosity Function ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mass Relation ◽  
Line Profiles ◽  
Star Formation Histories ◽  
Number Counts ◽  
Formation Efficiency ◽  
Mass Functions

AbstractWe present an empirical model built on a high-resolution N-body dark matter simulation. We assume a redshift-independent star-formation efficiency for each halo to convert the accretion rate into a star-formation rate. Our model is calibrated using the z = 4 UV luminosity function (UVLF) and successfully predicts the observed UVLF at z = 5 – 10. We present predictions at z = 5 – 10 for UV luminosity and stellar mass functions, JWST number counts, the stellar-to-halo mass relation and star-formation histories. We combine this model with bleeding-edge reionization constraints (from z > 7 quasars, z ∼ 7 Ly α line-profiles, the updated Planck τ) to find new perspectives on the Epoch of Reionization (EoR). We find MUV < − 13.5 galaxies need an average fesc = 0.22 ± 0.05 to drive reionization and a highly compressed timeline: the IGM neutral fraction is [0.9, 0.5, 0.1] at z = [8.4 ± 0.2, 7.0 ± 0.2, 6.3 ± 0.2]. Inspired by the newly assembled sample of Lyman Continuum leakers that unanimously displays higher-than-average star-formation surface density (sigma), we fit a model tying fesc to sigma. Since sigma grows by > 2.5 dex over z = 0 – 8, our model explains the humble values of fesc at low-z. We find, strikingly, that < 5% of galaxies with MUV < − 18 account for > 80% of the reionization budget. We predict leakers like COLA1 (z = 6.6, MUV = − 21.5) become common towards the EoR and that the protagonists of reionization are not hiding across the faint-end of the luminosity function but are already known to us.

scholarly journals THE MASS FUNCTION OF DARK MATTER HALOES IN A COSMOLOGICAL MODEL WITH A RUNNING PRIMORDIAL POWER SPECTRUM

2005 ◽  
Vol 14 (08) ◽  
pp. 1305-1312
Author(s):  
TONG-JIE ZHANG ◽  
HONG LIANG ◽  
WEN-ZHONG LIU ◽  
BAO-QUAN WANG
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Mass Function ◽  
Small Mass ◽  
Cluster Of Galaxies ◽  
Primordial Power Spectrum ◽  
Power Spectral ◽  
Halo Masses ◽  
Mass Functions ◽  
The Universe

We present the first study on the mass functions of Jenkins et al. (J01) and an estimate of their corresponding largest virialized dark halos in the Universe for a variety of dark-energy cosmological models with a running spectral index. Compared with the PL–CDM model, the RSI–CDM model can raise the mass abundance of dark halos for small mass halos at lower redshifts, but it is not apparent on scales of massive mass halos. Particularly, this discrepancy increases largely with the decrease of redshift, and the RSI–CDM model can suppress the mass abundance on any scale of halo masses at higher redshift. As for the largest mass of virialized halos, the spatially flat ΛCDM models give more massive mass of virialized objects than other models for both of PL–CDM and RSI–CDM power spectral indexs, and the RSI–CDM model can enhance the mass of largest virialized halos for all of models considered in this paper. So we probably distinguish the PL–CDM and RSI–CDM models by the largest virialized halos in the future survey of cluster of galaxies.

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