About

Upcoming weak lensing surveys require a detailed theoretical understanding of the matter power spectrum in order to derive accurate and precise cosmological parameter values. While galaxy formation is known to play an important role, its precise effects are currently unknown. To address this, we (Marcel van Daalen, Ian McCarthy and Joop Schaye) collected 92 matter power spectra from the OWLS, cosmo-OWLS and BAHAMAS simulation suites, including different LCDM cosmologies, neutrino masses, subgrid prescriptions and AGN feedback strengths.

Many of these power spectra were compared and discussed in van Daalen, McCarthy & Schaye (2019, accepted), a follow-up on van Daalen et al. (2011). Some of our main findings were that changing the strength of AGN feedback has a major effect on the matter power spectrum, and that changing the strength of supernova feedback in the presence of AGN feedback can significantly affect the power on large scales as well. Most importantly, we found that the effect of galaxy formation on large scales, k<1h/Mpc, is strongly correlated with the baryon fraction in group-scale haloes. Differences in this quantity can explain the differences seen between the predictions of different simulations for the large-scale power in the presence of baryons. In the paper, we present a fitting function that predicts the effect of galaxy formation on the matter power spectrum to within 1% for k<1h/Mpc as a function of only the mean baryon fraction in 1014M haloes.

The 92 power spectra in our power spectrum library can be found here.

The data

Links to the library of matter power spectra from 92 simulations are below. Most simulation power spectra are available down to k>10 h/Mpc and redshifts between 0 and 3, but all simulations will have power spectra at z=0 at the very least. Next to the power spectra for each hydrodynamical simulation simulation is a link to the power spectra for its dark matter only counterpart. For more information, see tables 1 and 2 in van Daalen, McCarthy & Schaye (2019). All power spectra are total matter power spectra, which includes massive neutrinos where applicable, and shot noise was subtracted. CDM-only power spectra can be found here.

Hydro sim DMO sim
BAHAMAS_Theat7.6_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_Theat8.0_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_nu0.06_Planck2015 DMONLY_2fluid_nu0.06_Planck2015_L400N1024
BAHAMAS_nu0.06_WMAP9 DMONLY_2fluid_nu0.06_WMAP9_L400N1024
BAHAMAS_nu0.12_Planck2015 DMONLY_2fluid_nu0.12_Planck2015_L400N1024
BAHAMAS_nu0.12_WMAP9 DMONLY_2fluid_nu0.12_WMAP9_L400N1024
BAHAMAS_nu0.24_Planck2015 DMONLY_2fluid_nu0.24_Planck2015_L400N1024
BAHAMAS_nu0.24_WMAP9 DMONLY_2fluid_nu0.24_WMAP9_L400N1024
BAHAMAS_nu0.48_Planck2015 DMONLY_2fluid_nu0.48_Planck2015_L400N1024
BAHAMAS_nu0.48_WMAP9 DMONLY_2fluid_nu0.48_WMAP9_L400N1024
BAHAMAS_nu0_BAO_L200N512 DMONLY_nu0_BAO_L200N512
BAHAMAS_nu0_Planck2013 DMONLY_2fluid_nu0_Planck2013_L400N1024
BAHAMAS_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_nu0_WMAP9_L100N512 DMONLY_2fluid_nu0_WMAP9_L100N512
BAHAMAS_nu0_WMAP9_v2 DMONLY_2fluid_nu0_v2_WMAP9_L400N1024
BAHAMAS_nu0_WMAP9_v3 DMONLY_2fluid_nu0_v3_WMAP9_L400N1024
C-OWLS_AGN_Mseed800_Theat8.5_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Mseed800_Theat8.7_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Mseed800_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.3_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_Theat8.5_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.5_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_Theat8.5_WMAP7_L100N256 DMONLY_WMAP7_L100N256
C-OWLS_AGN_Theat8.5_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Theat8.7_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.7_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_WMAP7_L200N1024 DMONLY_WMAP7_L200N1024
C-OWLS_AGN_WMAP7_L200N512 DMONLY_WMAP7_L200N512
C-OWLS_NOCOOL_UVB_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_NOCOOL_UVB_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_NOCOOL_UVB_WMAP7_L100N256 DMONLY_WMAP7_L100N256
C-OWLS_NOCOOL_UVB_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_NOCOOL_UVB_WMAP7_L200N512 DMONLY_WMAP7_L200N512
C-OWLS_REF_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_REF_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_REF_WMAP7_L200N1024 DMONLY_WMAP7_L200N1024
C-OWLS_REF_WMAP7_L200N512 DMONLY_WMAP7_L200N512
OWLS_AGN DMONLY_L100N512
OWLS_AGN_LOBETA DMONLY_L100N512
OWLS_AGN_LOBETA_NOSN DMONLY_L100N512
OWLS_AGN_LOBETA_Theat7.0 DMONLY_L100N512
OWLS_AGN_WMAP7 DMONLY_WMAP7_L100N512
OWLS_AGN_WMAP7_CAMB DMONLY_WMAP7_CAMB_L100N512
OWLS_AGN_WMAP7_L100N256 DMONLY_WMAP7_L100N256
OWLS_DBLIMFCONTSFML14 DMONLY_L100N512
OWLS_DBLIMFCONTSFV1618 DMONLY_L100N512
OWLS_DBLIMFV1618 DMONLY_L100N512
OWLS_EOS1p0 DMONLY_L100N512
OWLS_IMFSALP DMONLY_L100N512
OWLS_NOAGB_L100N256 DMONLY_L100N256
OWLS_NOAGB_NOSNIa DMONLY_L100N512
OWLS_NONRAD DMONLY_L100N512
OWLS_NOSN DMONLY_L100N512
OWLS_NOSN_NOZCOOL DMONLY_L100N512
OWLS_NOZCOOL DMONLY_L100N512
OWLS_REF DMONLY_L100N512
OWLS_REF_L100N256 DMONLY_L100N256
OWLS_REF_WMAP7 DMONLY_WMAP7_L100N512
OWLS_REF_WMAP7_L100N256 DMONLY_WMAP7_L100N256
OWLS_SNIaGAUSS DMONLY_L100N512
OWLS_WDENS DMONLY_L100N512
OWLS_WML1V848 DMONLY_L100N512
OWLS_WML4 DMONLY_L100N512
OWLS_WPOTNOKICK DMONLY_L100N512
OWLS_WTHERMAL_WMAP5 DMONLY_WMAP5_L100N512
OWLS_WVCIRC DMONLY_L100N512

The data - CDM-only

Links to cold dark matter power spectra are below. Shot noise was subtracted. Note that for many simulations, only z=0 is available.

Hydro sim DMO sim
BAHAMAS_Theat7.6_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_Theat8.0_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_nu0.06_Planck2015 DMONLY_2fluid_nu0.06_Planck2015_L400N1024
BAHAMAS_nu0.06_WMAP9 DMONLY_2fluid_nu0.06_WMAP9_L400N1024
BAHAMAS_nu0.12_Planck2015 DMONLY_2fluid_nu0.12_Planck2015_L400N1024
BAHAMAS_nu0.12_WMAP9 DMONLY_2fluid_nu0.12_WMAP9_L400N1024
BAHAMAS_nu0.24_Planck2015 DMONLY_2fluid_nu0.24_Planck2015_L400N1024
BAHAMAS_nu0.24_WMAP9 DMONLY_2fluid_nu0.24_WMAP9_L400N1024
BAHAMAS_nu0.48_Planck2015 DMONLY_2fluid_nu0.48_Planck2015_L400N1024
BAHAMAS_nu0.48_WMAP9 DMONLY_2fluid_nu0.48_WMAP9_L400N1024
BAHAMAS_nu0_Planck2013 DMONLY_2fluid_nu0_Planck2013_L400N1024
BAHAMAS_nu0_WMAP9 DMONLY_2fluid_nu0_WMAP9_L400N1024
BAHAMAS_nu0_WMAP9_L100N512 DMONLY_2fluid_nu0_WMAP9_L100N512
BAHAMAS_nu0_WMAP9_v2 DMONLY_2fluid_nu0_v2_WMAP9_L400N1024
BAHAMAS_nu0_WMAP9_v3 DMONLY_2fluid_nu0_v3_WMAP9_L400N1024
C-OWLS_AGN_Mseed800_Theat8.5_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Mseed800_Theat8.7_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Mseed800_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.3_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_Theat8.5_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.5_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_Theat8.5_WMAP7_L100N256 DMONLY_WMAP7_L100N256
C-OWLS_AGN_Theat8.5_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_AGN_Theat8.7_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_AGN_Theat8.7_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_AGN_WMAP7_L200N1024 DMONLY_WMAP7_L200N1024
C-OWLS_AGN_WMAP7_L200N512 DMONLY_WMAP7_L200N512
C-OWLS_NOCOOL_UVB_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_NOCOOL_UVB_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_NOCOOL_UVB_WMAP7_L100N256 DMONLY_WMAP7_L100N256
C-OWLS_NOCOOL_UVB_WMAP7_L100N512 DMONLY_WMAP7_L100N512
C-OWLS_NOCOOL_UVB_WMAP7_L200N512 DMONLY_WMAP7_L200N512
C-OWLS_REF_Planck2013 DMONLY_Planck2013_L400N1024
C-OWLS_REF_WMAP7 DMONLY_WMAP7_L400N1024
C-OWLS_REF_WMAP7_L200N1024 DMONLY_WMAP7_L200N1024
C-OWLS_REF_WMAP7_L200N512 DMONLY_WMAP7_L200N512
OWLS_AGN DMONLY_L100N512
OWLS_AGN_LOBETA DMONLY_L100N512
OWLS_AGN_LOBETA_NOSN DMONLY_L100N512
OWLS_AGN_LOBETA_Theat7.0 DMONLY_L100N512
OWLS_AGN_WMAP7 DMONLY_WMAP7_L100N512
OWLS_AGN_WMAP7_CAMB DMONLY_WMAP7_CAMB_L100N512
OWLS_AGN_WMAP7_L100N256 DMONLY_WMAP7_L100N256
OWLS_DBLIMFCONTSFML14 DMONLY_L100N512
OWLS_DBLIMFCONTSFV1618 DMONLY_L100N512
OWLS_DBLIMFV1618 DMONLY_L100N512
OWLS_EOS1p0 DMONLY_L100N512
OWLS_IMFSALP DMONLY_L100N512
OWLS_NOAGB_NOSNIa DMONLY_L100N512
OWLS_NONRAD DMONLY_L100N512
OWLS_NOSN DMONLY_L100N512
OWLS_NOSN_NOZCOOL DMONLY_L100N512
OWLS_NOZCOOL DMONLY_L100N512
OWLS_REF DMONLY_L100N512
OWLS_REF_L100N256 DMONLY_L100N256
OWLS_REF_WMAP7 DMONLY_WMAP7_L100N512
OWLS_REF_WMAP7_L100N256 DMONLY_WMAP7_L100N256
OWLS_SNIaGAUSS DMONLY_L100N512
OWLS_WDENS DMONLY_L100N512
OWLS_WML1V848 DMONLY_L100N512
OWLS_WML4 DMONLY_L100N512
OWLS_WTHERMAL_WMAP5 DMONLY_WMAP5_L100N512
OWLS_WVCIRC DMONLY_L100N512

The paper

Exploring the effects of galaxy formation on matter clustering through a library of simulation power spectra
Marcel P. van Daalen, Ian G. McCarthy and Joop Schaye
2019, accepted by MNRAS [ADS] [astro-ph]
Abstract: Upcoming weak lensing surveys require a detailed theoretical understanding of the matter power spectrum in order to derive accurate and precise cosmological parameter values. While galaxy formation is known to play an important role, its precise effects are currently unknown. We present a set of 92 matter power spectra from the OWLS, cosmo-OWLS and BAHAMAS simulation suites, including different LCDM cosmologies, neutrino masses, subgrid prescriptions and AGN feedback strengths. We conduct a detailed investigation of the dependence of the relative difference between the total matter power spectra in hydrodynamical and collisionless simulations on the effectiveness of stellar and AGN feedback, cosmology and redshift. The strength of AGN feedback can greatly affect the power on a range of scales, while a lack of stellar feedback can greatly increase the effectiveness of AGN feedback on large scales. We also examine differences in the initial conditions of hydrodynamic and N-body simulations that can lead to a ∼ 1% discrepancy in the large-scale power, and furthermore show our results to be insensitive to cosmic variance. We present an empirical model capable of predicting the effect of galaxy formation on the matter power spectrum at z=0 to within 1% for k<1h/Mpc, given only the mean baryon fraction in galaxy groups. Differences in group baryon fractions can also explain the quantitative disagreement between predictions from the literature. All total and dark matter only power spectra in this library will be made publicly available here.

Contact

If you have any questions about the paper, model or data, please fill in the form below.

  • daalen [at] strw.leidenuniv.nl