UV luminosity functions

Mason, Trenti & Treu (2015, 2022) UV luminosity function model 0 <= z <= 20

LF/ contains the UV LF model, both with and without dust attenuation and for ST and Reed+07 hmf (see Assumptions below). Uncertainties are approx. 0.2-0.4 dex based on the calibration at z~5 (I would assume 0.2 dex at z<9, 0.3 dex at 9 < z < 13 and 0.4 dex at z>13). Columns are:
1. Muv[mag]
2. log10_Phi_max (100% efficiency LF)
3. log10_Phi_dust
4. log10_Phi_nodust Phi units are #/mag/Mpc^3.

e.g. to plot the 'dust' model below at z=12 using the Reed+07 hmf use

z = 12
LF = np.genfromtxt(f'../../UVLF_model/LF/LF_z={z}_Reed07.txt') 
plt.semilogy(LF[:,0], 10**LF[:,2])

MUV_Mh/ contains the UV magnitude - halo mass relation, both with and without dust attenuation Muv_Mh. Columns are:
1. logMh [Msun]
2. Muv[mag]
3. Muv_dust[Mag] (which includes dust attenuation following Mason+15 eqn 4)

Assumptions

We use hmf to calculate halo mass functions and use the Eisenstein & Hu 1998 (EH) transfer function as it works better than CAMB at high z
- We provide LFs calculated using both both Sheth-Tormen and Reed+07 halo mass functions. These are almost identical at z<10, but at z>10 ST predicts a higher abundance of massive halos. Reed+07 hmfs were derived using N-body simulations at z~10-30.
Flat LCDM cosmology with h=0.7, Om0=0.3,
For z<10 we use metallicity = 0.02 Z_sun, z>=10 we use Z = 0.01 Z_sun

If you use these models please include a citation to Mason, Trenti & Treu (2015) (for z < 10) and Mason, Trenti & Treu (2022) (for z >= 10).