Small-scale galaxy clustering in the eagle simulation

Artale, M. Celeste; Pedrosa, Susana; Trayford, James W.; Theuns, Tom; Farrow, Daniel J.; Norberg, Peder; Zehavi, Idit; Bower, Richard G.; Schaller, Matthieu

doi:10.1093/mnras/stx1263

Cited by 37 publications

(36 citation statements)

References 115 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…galaxy specific starformation rate distributions, passive fractions and the TullyFisher relation; Schaye et al 2015) that are not explicitly used in the calibration. Artale et al (2017) also find good agreement between the clustering of blue galaxies in EAGLE and those in the GAMA survey, concluding that these simulated and observed galaxies with similar properties occupy dark matter haloes of similar masses.…”

Section: Overview Of the Eagle Simulationsupporting

confidence: 63%

The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8–2.2, with HiZELS

Cochrane

Best

Sobral

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8-2.2, with HiZELS' Monthly Notices of the Royal Astronomical Society, vol. 475, no. 3, General rightsCopyright for the publications made accessible via the Edinburgh Research Explorer is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policyThe University of Edinburgh has made every reasonable effort to ensure that Edinburgh Research Explorer content complies with UK legislation. If you believe that the public display of this file breaches copyright please contact openaccess@ed.ac.uk providing details, and we will remove access to the work immediately and investigate your claim. ABSTRACTThe deep, near-infrared narrow-band survey HiZELS has yielded robust samples of Hα-emitting star-forming galaxies within narrow redshift slices at z = 0.8, 1.47 and 2.23. In this paper, we distinguish the stellar mass and star-formation rate (SFR) dependence of the clustering of these galaxies. At high stellar masses (M * /M 2 × 10 10 ), where HiZELS selects galaxies close to the so-called star-forming main sequence, the clustering strength is observed to increase strongly with stellar mass (in line with the results of previous studies of mass-selected galaxy samples) and also with SFR. These two dependencies are shown to hold independently. At lower stellar masses, however, where HiZELS probes high specific SFR galaxies, there is little or no dependence of the clustering strength on stellar mass, but the dependence on SFR remains: high-SFR low-mass galaxies are found in more massive dark matter haloes than their lower SFR counterparts. We argue that this is due to environmentally driven star formation in these systems. We apply the same selection criteria to the EAGLE cosmological hydrodynamical simulations. We find that, in EAGLE, the high-SFR low-mass galaxies are central galaxies in more massive dark matter haloes, in which the high SFRs are driven by a (halo-driven) increased gas content.

show abstract

Section: Overview Of the Eagle Simulationsupporting

confidence: 63%

The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8–2.2, with HiZELS

Cochrane

Best

Sobral

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Cosmological hydrodynamical simulations are starting to play a major role in the study of galaxy formation and evolution. Comparisons of such simulations with observations show broad agreement (e.g., Vogelsberger et al 2014;Schaye et al 2015;Artale et al 2017).…”

Section: Introductionmentioning

confidence: 63%

The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos

Zehavi

Contreras

Padilla

et al. 2018

ApJ

Self Cite

152

150

View full text Add to dashboard Cite

We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto-and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.

show abstract

“…We note also that our simulations do not take into account the effects of baryon physics that can modify the matter distribution and the properties of haloes measured from DM-only simulations, see e.g. [73][74][75][76][77][78][79]. As in nCDM models, the thermal inflation model predicts fewer low-mass haloes and sub-haloes than standard ΛCDM, but without involving any modification to the dark matter sector.…”

Section: Discussionmentioning

confidence: 96%

N-body simulations of structure formation in thermal inflation cosmologies

Leo

Baugh

et al. 2018

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Thermal inflation models (which feature two inflationary stages) can display damped primordial curvature power spectra on small scales which generate damped matter fluctuations. For a reasonable choice of parameters, thermal inflation models naturally predict a suppression of the matter power spectrum on galactic and sub-galactic scales, mimicking the effect of warm or interacting dark matter. Matter power spectra in these models are also characterised by an excess of power (with respect to the standard ΛCDM power spectrum) just below the suppression scale. By running a suite of N-body simulations we investigate the non-linear growth of structure in models of thermal inflation. We measure the non-linear matter power spectrum and extract halo statistics, such as the halo mass function, and compare these quantities with those predicted in the standard ΛCDM model and in other models with damped matter fluctuations. We find that the thermal inflation models considered here produce measurable differences in the matter power spectrum from ΛCDM at redshifts z > 5 for wavenumbers k ∈ [2, 64] h Mpc −1 , while the halo mass functions are appreciably different at all redshifts in the halo mass range M halo ∈ [10 9 , 10 12 ] h −1 M resolved by our simulations. The halo mass function at z = 0 for thermal inflation displays an enhancement of around ∼ 20% with respect to ΛCDM and a damping at lower halo masses, with the position of the enhancement depending on the value of the free parameter in the model. The enhancement in the halo mass function (with respect to ΛCDM ) increases with redshift, reaching ∼ 40% at z = 5. We also study the accuracy of the analytical Press-Schechter approach, using different filters to smooth the density field, to predict halo statistics for thermal inflation. We find that the predictions with the smooth-k filter we proposed in a separate paper agree with the simulation results over a wider range of halo masses than is the case with other filters commonly used in the literature.

show abstract

Small-scale galaxy clustering in the eagle simulation

Cited by 37 publications

References 115 publications

The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8–2.2, with HiZELS

The dependence of galaxy clustering on stellar mass, star-formation rate and redshift at z = 0.8–2.2, with HiZELS

The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos

N-body simulations of structure formation in thermal inflation cosmologies

Contact Info

Product

Resources

About