Simulation organization

Here is a quick table of what simulations are publicly available and how the file-names map to each simulations type. All sims except the Fiducial runs, have a p and m version, which denotes whether they are a shift up/down from the fiducial in a given parameter. For the inflationary models, the parameter is fNL. Note that we separate the tables for the inflationary runs in our recent works and the Quijote-derived runs from the original paper as the former share no random seeds with Quijote whereas the latter are a precise match to Quijote and so can be used in tandem.

Ulagam 2025

These simulations are independent of Quijote and resolve a variety of primordial signatures, including cosmological collider models. We have 10 runs per model. For space reasons, not every single model from the papers were uploaded for this initial release. Please contact me if you’d like a particular model!

Folder name	Descriptions
Gauss_fid	Gaussian simulations (fNL = 0) with same random seed as the others. Useful for variance cancellation.
Local	Local-type
Equilateral	Equilateral-type
Orthogonal	Orthogonal type, using the first, simpler template of Senatore. In Quijote this is called OR-CMB.
QSF_{nu}	Simulations of the Quasi Single Field model. nu is the mass in Hubble units.
SI_{mu}	Simulations of the Scalar-I template. mu is the mass in Hubble units.
SII_{mu}	Simulations of the Scalar-II template. mu is the mass in Hubble units.
HSC_{s}	Simulations of the heavy-spin collider. s is the (integer) spin.
LSC_{-logalpha}	Simulations of the low-speed collider. alpha is a scaling parameter set by sound speed and particle mass. LSC_0 corresponds to alpha = 1; LSC_3 corresponds to alpha = 1e-3.
MSC_{-logc1…}	Simulations of the multi-speed collider. MSC_110 is c1 = c2 = 1e-1 and c3 = 1; MSC_200 is c1 = 1e-2, c2 = c3 = 1, for example.
LSD_SF_{n}	Scale-dependent local PNG with n the spectral index. Assumes only a single field exhibits scale dependence.
LSD_MF_{n}	Scale-dependent local PNG with n the spectral index. Assumes multiple fields exhibit scale dependence.
LINRES_{w}	Linear resonance bispectrum, with w the frequency.
LOGRES_{w}	Logarithmic resonance bispectrum, with w the frequency.
K2COSRES_w{w}_a{alpha}	K2cos mode of Adshead++. The frequency w and damping scale alpha are free parameters.
NBD2_{kc}	NBD-mode 2 (Planck). The characteristic scale kc is varied between 0.1, 0.2, and 0.6 (h/Mpc).
NBDsin_{w}	NBD-sin (Planck). w is the frequency.
LINRES_2_A{A}_w{w}	Both bispectrum and power-spectrum oscillations. The p and m still vary fNL. We provide A values of -1 and 1. w is the frequency of P(k) oscillations only (bispectrum frequency fixed at 2).
LOGRES_2_A{A}_w{w}	Same as above but for logarithmic resonance (oscillations in P(k) are in log(k), consistent with the bispectrum).

Ulagam 2023

All simulations below use the initial conditions from Quijote. So simulation under index 3 is the same as the simulation under index 3 in Quijote as well. We have verified the density fields are consistent. We have 2600 fiducial runs and 100 runs at the other setups.

Folder	Descriptions
fiducial	Simulations at fiducial cosmology, using Quijote initial conditions.
Om	Variation in matter energy density fraction, Omega_m.
s8	Variation in rms amplitude of fluctuations at z = 0, sigma_8.
ns	Variation in primordial spectral tilt, n_s.
w	Variation in dark energy equation of state.
LC	Local-type non-Gaussianity.
EQ	Equilateral-type non-Gaussianity.
OR_CMB	Orthogonal-type non-Gaussianity using the original Senatore template (incorrect squeezed-limit scaling).
OR_LSS	Orthogonal-type non-Gaussianity using the modified Senatore template (correct squeezed-limit scaling).