Halo models of large scale structure

Cooray, Asantha; Sheth, Ravi K.

doi:10.1016/s0370-1573(02)00276-4

Cited by 2,000 publications

(2,517 citation statements)

References 281 publications

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“…The clustering of galaxies at high-redshift provides a valuable constraint on their dark matter halo masses and their occupation number, especially in the context of the halo model for large-scale structure galaxy distribution (Cooray & Sheth, 2002). The halo mass scale of DSFGs is helpful to understand the mass scale at which starbursts are frequently found and can be compared to theoretical and numerical predictions related to efficient gas-cooling in dark matter halos (Dekel et al, 2009a,b;Behroozi et al, 2013).…”

Section: Clustering Of Dsfgsmentioning

confidence: 99%

“…This figure is reproduced from Thacker et al (2013) with permission from the authors and AAS. the ansatz of the halo model (Cooray & Sheth, 2002) the faint galaxy clustering captures the statistics on how they occupy the dark matter halos in the universe. The resulting anisotropies of the CIB are then a reflection of the spatial clustering of dark matter halos that are hosted by faint DSFGs and the total CIB intensity produced by those galaxies.…”

Section: Clustering Of Faint Unresolved Dsfgs Through the Cib Anisotmentioning

confidence: 99%

“…To separate intrinsic clustering from this magnification effect, the magnification-induced cross-correlation is best measured with samples of foreground galaxies and background DSFGs that do not overlap in redshift. When combined with the number counts, such a cross-correlation study can provide constraints on cosmological parameters and galaxy bias, a key ingredient in galaxy formation and evolution models Cooray & Sheth (2002);Jain (2002).…”

Section: Cib Power Spectrummentioning

confidence: 99%

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Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Clustering Of Dsfgsmentioning

confidence: 99%

Section: Clustering Of Faint Unresolved Dsfgs Through the Cib Anisotmentioning

confidence: 99%

Section: Cib Power Spectrummentioning

confidence: 99%

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Dusty star-forming galaxies at high redshift

2014

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“…In our calculation we follow Cooray and Sheth [35] for b(M, z) and Eisenstein and Hu [36] for P lin . The mass function, dn/dM is given by:…”

Section: A the Synchrotron Anisotropy Calculationmentioning

confidence: 99%

Anisotropy of the extragalactic radio background from dark matter annihilation

Fang

Linden

2015

Phys. Rev. D

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Observations of the extragalactic radio background have uncovered a significant isotropic emission across multiple frequencies spanning from 22 MHz to 10 GHz. The intensity of this non-thermal emission component significantly exceeds the expected contribution from known astrophysical sources. Interestingly, models have indicated that the annihilation of dark matter particles may reproduce both the flux and spectrum of the excess. However, the lack of a measurable anisotropy in the residual emission remains challenging for both dark matter and standard astrophysical interpretations of the ARCADE-2 data. We calculate the expected synchrotron anisotropy from dark matter annihilation and show that these models can produce very small anisotropies, though this requires galaxy clusters to have large substructure contributions and strong magnetic fields. We show that this constraint can be significantly relaxed, however, in scenarios where electrons produced via dark matter annihilation can be efficiently reaccelerated by Alfvén waves in the intra-Cluster medium. Our analysis indicates that any source capable of explaining the intensity and isotropy of the extragalactic radio excess must have a spatial extension far larger than typical for baryons in galaxies, hinting at a novel physics interpretation.

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“…We can therefore infer the link between galaxies and dark matter haloes directly from the observed clustering properties of galaxies. The halo based description is the backbone of this approach and provides a simple and natural way of modelling the difference between the clustering of galaxies relative to dark matter in the form of the halo model (Cooray & Sheth 2002). …”

Section: Introductionmentioning

confidence: 99%

How does clustering depend on environment?

Abbas

Sheth

2004

IAU

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Abstract. According to the current paradigm, galaxies form and reside in extended cold dark matter (CDM) halos and in turn are key tracers of cosmological structure. Understanding how different types of galaxies occupy halos of different masses is one of the major challenges facing extragalactic astrophysics. The observed galaxy properties depend on the environment surrounding the galaxy. Within the framework of most galaxy formation models the environmental dependence of the galaxy population is mainly due to the change of the halo mass function with large-scale environment. Such models make precise predictions for how galaxy clustering should depend on environment. We will illustrate this by presenting analytical models of dark matter and galaxy clustering along with results obtained from numerical simulations. With these results we can hope to obtain a better understanding of the link between galaxies and dark matter and thereby constrain galaxy formation models.

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Halo models of large scale structure

Cited by 2,000 publications

References 281 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Anisotropy of the extragalactic radio background from dark matter annihilation

How does clustering depend on environment?

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