Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations

Rodríguez-Puebla, Aldo; Behroozi, Peter; Primack, Joel R.; Klypin, Anatoly; Lee, Christoph I.; Hellinger, Doug

doi:10.1093/mnras/stw1705

Cited by 245 publications

(253 citation statements)

References 117 publications

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“…Each column reflects a different halo mass range, while each row reflects a different halo property. We chose mass bins such that we could compare halos below, at, and above the characteristic mass M C of halos that are collapsing at z = 0, which is 10 12.70 M = 5.0 × 10 12 M for the Planck cosmological parameters used in the Bolshoi-Planck simulation (see Rodríguez-Puebla et al 2016, Figure 9, for a plot showing M C as a function of redshift). For each panel, different lines represent different smoothing radii used to determine the local density around halos.…”

Section: Correlations At the Present Epochmentioning

confidence: 99%

Properties of dark matter haloes as a function of local environment density

Lee

Primack

Behroozi

et al. 2016

Mon. Not. R. Astron. Soc.

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We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 h −1 Mpc. We find that low mass halos (those less massive than the characteristic mass M C of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts z < 1, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.

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Section: Correlations At the Present Epochmentioning

confidence: 99%

Properties of dark matter haloes as a function of local environment density

Lee

Primack

Behroozi

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We have adopted a baryon fraction of 0.1578. Our cosmology is consistent with the Planck 2013 results (Planck Collaboration et al 2014) and was chosen to match that of the Bolshoi Planck simulation (Rodriguez-Puebla et al 2016). We use CANDELS mock lightcones (Somerville et al in prep.…”

Section: The Semi-analytic Modelmentioning

confidence: 99%

“…We use CANDELS mock lightcones (Somerville et al in prep. ) extracted from the Bolshoi Planck dark-matter N-body simulation Trujillo-Gomez et al 2011;Rodriguez-Puebla et al 2016). The ROCKSTAR algorithm of Behroozi et al (2013a) is used to identify dark matter halos.…”

Section: The Semi-analytic Modelmentioning

confidence: 99%

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Brennan

Pandya

Somerville

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the correlation of galaxy structural properties with their location relative to the SFR-M * correlation, also known as the star formation "main sequence" (SFMS), in the CANDELS and GAMA surveys and in a semi-analytic model (SAM) of galaxy formation. We first study the distribution of median Sérsic index, effective radius, star formation rate (SFR) density and stellar mass density in the SFR-M * plane. We then define a redshift dependent main sequence and examine the medians of these quantities as a function of distance from this main sequence, both above (higher SFRs) and below (lower SFRs). Finally, we examine the distributions of distance from the main sequence in bins of these quantities. We find strong correlations between all of these galaxy structural properties and the distance from the SFMS, such that as we move from galaxies above the SFMS to those below it, we see a nearly monotonic trend towards higher median Sérsic index, smaller radius, lower SFR density, and higher stellar density. In the semi-analytic model, bulge growth is driven by mergers and disk instabilities, and is accompanied by the growth of a supermassive black hole which can regulate or quench star formation via Active Galactic Nucleus (AGN) feedback. We find that our model qualitatively reproduces the trends described above, supporting a picture in which black holes and bulges co-evolve, and AGN feedback plays a critical role in moving galaxies off of the SFMS.

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“…To calculate M * , we follow a similar procedure of the one presented in Rodríguez-Puebla et al 2016 to calculate the characteristic mass of halos just collapsing at redshift z (M C ). This is shown in Appendix A.…”

Section: Evolution In the Direction Of The Am Vectormentioning

confidence: 99%

“…Here we present the procedure to calculate M * , following the work of (Rodríguez-Puebla et al 2016) for the calculation of M C :…”

Section: Appendix A: Calculation Of M *mentioning

confidence: 99%

Angular momentum evolution in dark matter haloes: a study of the Bolshoi and Millennium simulations

Contreras

Padilla

Lagos

2017

Monthly Notices of the Royal Astronomical Society

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We use three different cosmological dark matter simulations to study how the orientation of the angular momentum vector (AM) in dark matter haloes evolve with time. We find that haloes in this kind of simulations are constantly affected by a spurious change of mass, which translates into an artificial change in the orientation of the AM. After removing the haloes affected by artificial mass change, we found that the change in the orientation of the AM vector is correlated with time. The change in its angle and direction (i.e. the angle subtended by the AM vector in two consecutive timesteps) that affect the AM vector has a dependence on the change of mass that affects a halo, the time elapsed in which the change of mass occurs and the halo mass. We create a Monte-Carlo simulation that reproduces the change of angle and direction of the AM vector. We reproduce the angular separation of the AM vector since a look back time of 8.5 Gyrs to today ( α) with an accuracy of approximately 0.05 in cos(α). We are releasing this Monte-Carlo simulation together with this publication. We also create a Monte Carlo simulation that reproduces the change of the AM modulus. We find that haloes in denser environments display the most dramatic evolution in their AM direction, as well as haloes with a lower specific AM modulus. These relations could be used to improve the way we follow the AM vector in low-resolution simulations.

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Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations

Cited by 245 publications

References 117 publications

Properties of dark matter haloes as a function of local environment density

Properties of dark matter haloes as a function of local environment density

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Angular momentum evolution in dark matter haloes: a study of the Bolshoi and Millennium simulations

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